Mexico

12th Scientific AssemblyAugust 26-31, 2013

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International Association of Geomagnetism and AeronomyInternational Union of Geodesy and Geophysics

International Association of Geomagnetism and Aeronomy

International Union of Geodesy and Geophysics

Edited by: J. Jesús Silva Corona, Responsible publisher: Harald BöhnelCentro de Geociencias, Universidad Nacional Autónoma de MéxicoSeptember 2012

Table of ContentsForeword 1

Avant-propos 2Deadlines 3

Schedule of the working days 3Social Program 3

Abstract Submission 4Submission Information 4

Pre-Registration 4Sample Abstract 5

Grant Applications 6Registration Information 6

Registration Fees 6Exhibition 7

Methods of Payment 7Venue 7

Accommodation 8Sponsorship 8

Internet Access 8Invitation Letter 9

IAGA Summer School 9Joint Sessions 10

Division 1 19Division 2 26Division 3 28Division 4 33Division 5 35

ICDC and IDCH 39Programme Committee 40Liability and Insurance 41

Scientific Freedom Policy Statement 41Travel to Mérida 41

Hotel List 42Hotels map 44

A few words about Mexico 45The venue: Yucatán 45

History of Merida 46Division´s Activities per Day 48

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IAGA Meeting 2013

ForewordThe Local Organising Committee and the Mexico National Committee of IUGG have

the great pleasure to welcome you to the 11th Scientific Assembly of the International Association of Geomagnetism and Aeronomy (IAGA) which is held in Mérida Yucatán, Mexico from 26 to 31 August 2013 with the motto: “Living on a Magnetic Planet”. Our Magnetic Planet Capricious (Changeable or Unpredictable) Field.

INTERNATIONAL ASSOCIATION OF GEOMAGNETISM AND AERONOMY (IAGA)

The International Association of Geomagnetism and Aeronomy (IAGA) is one of the eight associations of the International Union of Geodesy and Geophysics (IUGG). IAGA has a long history and can trace its origins to the commission for Terrestrial Magnetism and Atmospheric Electricity, part of the International Meteorological Organisation, which was established in 1873.

IAGA is a non-governmental body founded to promote and coordinate studies of the electrical and magnetic properties of the Earth’s core, mantle and crust, of the middle and upper atmosphere, of the ionosphere and magnetosphere, and the Sun, the solar wind, the planets and interplanetary bodies.

IAGA is organised into five Divisions and two Interdivisional (ID) commissions:Division I: Internal Magnetic FieldDivision II: Aeronomic PhenomenaDivision III: Magnetospheric PhenomenaDivision IV: Solar Wind and Interplanetary FieldDivision V: Geomagnetic Observatories, Surveys and AnalysesIDCH: Commission on HistoryICDC: Commission on Developing Countries.

Each Division and Commission is led by a Chair and Co-Chair. The Divisions and/or Commissions may form working Groups for topic areas and elect officers to run the busi-ness of the Working Groups. IAGA encourages free exchange of scientific information and facilitates international collaboration in research. IAGA holds an Ordinary General Assembly every four years in conjunction with each Ordinary General Assembly of IUGG. Between these General Assemblies, IAGA holds a Scientific Assembly sometimes with one of the other Associations of IUGG. In addition to these assemblies, IAGA organises workshops dedicated to specific topics. Through its assemblies and workshops, IAGA provides global forums for scientists to present and discuss their latest research results, to share knowledge, to establish standards, to resolve issues, and to promote interna-tional studies and cooperation.

The official languages of IAGA are English and French.

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Avant-proposLe Comite local d’organisation et le Comite National du Mexique de l’Union

Géodésique et Géophysique Internationale (UGGI) ont le grand plaisir de vous accueillir à la 12eme Assemblée Scientifique de l’Association Internationale de Géomagnétisme et d’Aéronomie (AIGA) qui se tient à Mérida Yucatán, Mexico, 26 – 31 /08 / 2013, ayant comme motto « Vivre sur une Planète magnétique »

ASSOCIATION INTERNATIONALE DE GEOMAGNETISME ET D’AERONOMIE (AIGA)

L’Association Internationale de Géomagnétisme et d’Aéronomie (AIGA) est une des huit associations de l’Union Géodésique et Géophysique Internationale (UGGI). L’AIGA a une longue histoire : elle a pour origine la Commission de magnétisme terrestre et d’électricité atmosphérique, qui faisait partie de l’Organisation météorologique interna-tionale, fondée en 1873.

L’AIGA est une organisation non gouvernementale fondée pour promouvoir l’étude des propriétés électriques et magnétiques de la Terre (noyau, manteau, croute), et de son environnement (moyenne et haute atmosphère, ionosphère et magnétosphère), du vent solaire, des planètes, de leurs satellites et des petits objets du système solaire.

L’AIGA est structurée en cinq Divisions et deux Commissions inter-divisions.Division I: Champs magnétiques internesDivision II: AéronomieDivision III: MagnétosphèreDivision IV: Vent solaire et champ magnétique interplanétaireDivision V: Observatoires géomagnétiques, lèves magnétiques et analyse de

donnéesCIDH (IDCH): Commission inter-division sur l’histoireCIPD (ICDC): Commission inter-division pour les pays en voie de développement

Chaque Division et Commission est placée sous la responsabilité d’un Président et d’un Vice-président. Elle peut former des Groupes de travail autour de thématiques spécifiques et élire des responsables charges de l’animation de ces groupes. Aux termes de ses statuts, l’AIGA a pour principaux objectifs de promouvoir l’échange gratuit d’infor-mations scientifiques et de faciliter la collaboration internationale dans son domaine de recherche. L’AIGA organise une Assemblée générale ordinaire tous les quatre ans, en même temps que chacune des Assemblées générales ordinaires de l’UGGI. Entre deux Assemblées générales, elle organise une Assemblée scientifique, parfois conjointement avec l’une ou l’autre des Associations membres de l’UGGI, ainsi que des symposiums spécialisés. Les Assemblées scientifiques et les symposiums organisés par l’AIGA constituent autant de forums dédiés à la présentation et à la discussion des travaux de recherche les plus récents, au partage des connaissances, à la définition de standards ainsi qu’à la promotion de programmes de recherche et de coopération internationaux.

Les langues officielles de l’AIGA sont l’anglais et le français.

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Schedule of the working daysMonday 26 to Saturday 31

08:30–10:00 Time Block 1 (oral sessions; Wednesday and Thursday Association lectures)10:00–10:30 Coffee break10:30–12:00 Time Block 2 (oral sessions)12:00–13:30 Lunch break

13:30–15:00 Time Block 3 (oral sessions)15:00–15:30 Coffee break15:30–17:00 Time Block 4 (oral sessions)17:00–19:00 Poster Block

The Exhibition area is open between 8:00–19:00. The session halls, poster sessions and exhibition areas are in the Fiesta Americana hotels (see map in page 44).

Social ProgramSunday, August 25 and September 1:

Guided City tours (included in the registration fee)Sunday evening, August 25:

Welcome reception (included in the registration fee)Between August 25–31:

Evening congress concerts (included in the registration fee)Wednesday evening, August 28:

Banquet (not included in the registration fee)Between August 24-September 1:

Bus excursions (not included in the registration fee)Other programs: August 25-31:

City Cultural events

Detailed information will be available on the IAGA 2013 web page and at the Information desk.

DeadlinesMarch 31, 2013 Grant application deadlineApril 13, 2013 Abstract submission deadlineApril 30, 2013 Decision about grantsMay 31, 2013 Reduced rate registrationJuly 1, 2013 Exhibition bookingAugust 20, 2013 Normal rate registrationCancellation deadlinesMay 31, 2013 Cancellation of registration with100% refundJuly 15, 2013 Cancellation of registration with 50% refundAfter July 15, 2013, No refund will be possible

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Pre-RegistrationA pre-registration is required to access the electronic abstract submission system

and for making any payments. The system will be available on the IAGA 2013 internet page.

Abstract SubmissionAbstract submission is only possible online (www.iaga2013.org.mx) before April,

2013. Acceptance e-mails will be sent before May 1, 2013. Submission of an abstract implies that IAGA has permission to reproduce it in programs and reports related to the Assembly. We expect that about 800 oral and 900 posters will be presented at the 12th IAGA Scientific Assembly. All oral talks will be 15 minutes long including 3 minutes for discussions. The posters format will be vertical, with a maximum width of 1m and a maximum height of 2m.

SUBMISSION INFORMATIONThe abstracts should be prepared in the following format:

a. ABSTRACT TITLE IN CAPITAL LETTERS, and leave a blank line after this lineb. Name(s) of Author(s): Left Justified, the First Name and the Last (Family) Name of the

Author WHO WILL PRESENT THE PAPER should be in capital letters.c. Affiliation(s) of the Author(s). In case of multiple affiliations, the number that corre-

sponds to the proper affiliation should be shown after each name. Leave a blank line after the last affiliation.

d. Text of Abstract: left justified, do not indent paragraphs, single line spacing, about 200–300 (max. 360) words in English or French. Below the abstract leave a blank line.

e. Please provide the following information:1. Symposium code,2. Symposium title,3. Keywords (1–3),4. Name and coordinates of the corresponding author,5. Type of presentation preferred (O for oral, P for poster, OP if the first prefer-

ence is oral, but the poster presentation is also acceptable),6. Equipment requested for presentation (PC for PC+digital projector, OH for

overhead projector. Indicate any special request.),7. Student paper: if a student author is presenting the paper, indicate YES,8. Are you applying for a grant? YES or NO after the name of each co-author,9. Message to Convener (if any).

Simple fonts (Times New Roman) and 12 letter size, and left-justification are recommended.

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Sample AbstractENVIRONMENTAL MAGNETISM AND TEQUILA PRODUCTION

SPEEDY GONZALEZ1, Jorge Preciozo2

1 Instituto de Magnetismo Ambiental, Tequila, Mexico, speego@tequila.net

2 Asociación de Tequileros de Jalisco, Guadalajara, Mexico, jpreciozo@tequila.jalisco.mx

Tequila was first produced in the 16th century near the location of the city of Tequila, where the Aztec people had previously made a fermented beverage from the agave plant, later popularly called pulque. When the Spanish conquistadors ran out of their own bran-dy, they began to distill agave to produce North America’s first indigenous distilled spirit. Planting, tending, and harvesting the agave plant remains a manual effort, largely unchanged by modern farm machinery and relying on centuries-old know-how. By regularly trimming any quiotes (a several-meter high stalk that grows from the center of the plant), the jima-dores prevent the agave from flowering and dying early, allowing it to fully ripen. The ji-madores must be able to tell when each plant is ready to be harvested, and using a special knife called a coa (with a circular blade on a long pole), carefully cut away the leaves from the piña (the succulent core of the plant). If harvested too late or too early, the piñas, which can average around 70 kilograms (150 lb) in the lowlands to 110 kilograms (240 lb) in the highlands, will not have the right amount of carbohydrates for fermentation.

After harvesting, the piñas are transported to ovens where they are slowly baked in order to break down their complex starches into simple sugars. Then the baked piñas are either shredded or mashed under a large stone wheel called a tahona. The pulp fiber, or bagazo, that is left behind is often reused as compost or animal feed, but can even be burnt as fuel or processed into paper. Some producers like to add a small amount of bagazo back into their fermentation tanks for a stronger agave flavor in the final product.

In this work we study the effect of the work in the fields by analyzing the magnetic prop-erties of the soil. Further, we study soils around the Tequila around the factory. Preliminary results indicate that Tequila production is highly beneficiary from the point view of contami-nation, and should be widely extended.

1. 1.12 2. Applied Rock Magnetism: Toward a better understanding of controlling factors of

environmental magnetic proxies3. environmental magnetism, contamination, Tequila4. Speedy Gonzalez, Instituto de Magnetismo Ambiental, Callejón sin salida 77, Tequila

46404, Mexico, e-mail: speego@tequila.net5. O6. PC7. NO8. Speedy Gonzalez: NO, Jorge Precioso: YES9. NONE

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Grant ApplicationsThe IAGA Executive Committee and the IAGA2013 LOC are working together to offer

a limited number of financial assistance grants to support participation at the 12th IAGA Scientific Assembly. An application for a grant can only be made by those who have submitted one or more abstracts to the scientific program. Financial assistance funds are limited and most awards will be for the registration fee only. It is unlikely that full support will be possible. Applications for grants should be sent exclusively to the Local Organizing Committee by e-mail to the address: loc@iaga2013.org.mx, with the subject: IAGA 2013, application for grant”. Already submitted abstract(s) by the applicant should be attached, together with a justification of the application. The deadline is strict (March 31, 2013), in order to be able to inform about the decision no later than April 30, 2013.

Registration InformationOnline registration is possible from autumn 2013. All participants are kindly request-

ed to pre-register online via the online database, by filling in their personal details.By using the online system, you can submit your abstracts, sign up for excursions,

pay the registration- and accommodation fees. All participants will receive a confirmation on registration and hotel reservation, but participants may check their own payment and reservation status in their personal records of the registration database.

Registration Fees

Category Reduced rate Normal rate On site rateBefore June 1, 2013 June 1 to Aug 22, 2013 Aug 23, 2013

Regular Participant1 US$ 390 US$ 430 US$ 470Young Scientist/Student Participant 1, 2

US$ 200 US$ 220 US$ 240

Accompanying person 3 US$ 100 US$ 110 US$ 130One day registration not possible not possible US$ 140

1 Registration fee for congress participants (regular and young scientist/student) include: participation in all sessions, admission to the exhibition, Abstract Volume on USB memory card, conference bag with printed Program Book, admission to the Opening and Closing ceremonies, welcome reception (August 25), congress social activities.

2 Category of young scientists (including students) has an exact age limit: it is 32 years Participants born in or after August 1981, and who are co-authors of at least one presen-tation submitted to the IAGA 2013, are eligible for this reduced registration fee.

3 Registered accompanying persons are entitled to receive: Admission to the Opening and Closing Ceremonies, Welcome reception (25 August), Congress social activities, Guided city walks in Mérida. A detailed program will be available on the IAGA 2013 internet page

The Banquet in the evening of 28 August and bus excursions are not included in any of these fees.

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Methods of PaymentEither by bank transfer to one of the accounts listed below:

In México (mexican pesos)

Account holder: UNAM Centro de Geociencias Bank: Santander (México) S.A.Account: 65-50350170-0CLABE: 014180655035017002Reference: Inscripciones IAGA 2013

International payments (USD)

Bank: J.P. Morgan Chase N.Y.Beneficiary bank: Santander S.A. BMSXMXMMAccount: 400047144Final beneficiary: UNAM, Centro de GeocienciasAccount: 6550350170-0SWIFT/ABA: 021000021

International payments (Euros)

Bank: Banco Santander Central Hispano MadridBeneficiary bank: Santander S.A. BMSXMXMMAccount: BMSXMXMMFinal beneficiary: UNAM, Centro de Geociencias Account: 6550350170-0SWIFT/ABA: BSCHESMMIBAN: ES2200495494802310148842

Or by major credit cards (American Express, Visa, MasterCard) using the secure online IAGA 2013 internet page.

If using bank transfer it is important to note “IAGA2013" and your registration ID and name. Registrations and hotel reservations, which are not accompanied by appropriate payment, will not be honored. Registrations and hotel reservations will be acknowledged in writing. Official invoices and receipts for fees paid by the participants can be sent by email or handed over in Mérida during on-site registration.

On-site registration fees, hotel charges and optional programs can be paid in cash in US dollars, Euros or Mexican Pesos at actual conversion rates indicated at the registra-tion desk, or by the credit cards listed above.

VenueThe IAGA 12th Scientific Assembly will be held in Fiesta Americana Hotel, at Paseo

de Montejo 451 and Av. Colón corner with Calle 60 (see map under “Hotel List”).

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ExhibitionAn indoor exhibition will be organized at the first floor of the Fiesta Americana hotel,

close to the poster area and coffee break services.Tea and coffee will be served within the exhibition area, thus ensuring maximum con-

tact between exhibitors and delegates. The Program Book will include a listing and brief description the services and products of each exhibiting company/organization. Each exhibiting company/organization will receive acknowledgement in all printed assembly materials including the Final Program and on signs prominently displayed at the registra-tion area. Each exhibiting company/organization will receive between one (1) and three (3) complimentary Full Registrations, according to the contracted booth size.

Indoor Exhibition (booth size):

4 m2 US$ 1200 12 m2 US$ 2800 (including 1 full registration) (including 2 full registrations)

8 m2 US$ 2000 16 m2 US$ 3600 (including 1 full registration) (including 3 full registrations)

All prices regarding exhibition and sponsorship include applicable taxes.In case that materials are required for exhibition (tables, chairs, electricity contacts,

etc), please contact the LOC. There are also possibilities for outdoor exhibitions, and potential exhibitors are kindly asked to contact the LOC (loc@iaga2013.org.mx)

SponsorshipBesides the exhibition, in our website you find detailed descriptions about other pos-

sibilities of involvement such as: sponsorship, delegate support, social program support, and advertising opportunities.

Sponsorship: Platinum Sponsor, Gold Sponsor, Silver Sponsor, Bronze Sponsor or Assembly Supporter.

Delegate Support: Assembly Bags, Delegate Notepaper & Pens, Delegate Name Badges, Internet Centre, Young Scientist Support.

Social Programme Support: Coffee Break(s), Welcome Reception, Cultural Event.

Advertising Opportunities: Advertising in the Program Booklet or Advertising Insert in Delegate Bag.

For all details of the Mérida IAGA Assembly see our website, www.iaga2013.org.mx.If you are interested in supporting the IAGA 2013, please contact the Local Organizing Committee (loc@iaga2013.org.mx).

AccommodationAccommodation has been reserved for conference participants and their companions

in Mérida hotels, as listed in our website, and at the end of this Circular. In order to re-serve accommodation, please reserve your room in the online database for Registration

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& Hotel Reservation before May 15, 2013. The reservation system will not offer dates prior to 21 August and after September 3, 2013. If you need to come earlier or depart later, or to share your room with somebody, please consult the organizers beforehand by e-mail, loc@iaga2013.org.mx. Paying 2 nights hotel fee − as a deposit − is mandatory. Without deposit the accommodation cannot be guaranteed.

Child Care Service

Child care services are available at Fiesta americana hotel and some others (see the Hotel list in pages 42 and 43).

Internet AccessA free wifi internet access is planned to be available to all participants in the session

area of the venue hotels. Some desktop computers will be available for those partici-pants, who do not have their own computer with themselves.

Invitation LetterIf you need a letter of invitation, please contact us after already having submitted your

pre-registration and abstract. This does not guarantee any visa to Mexico.

IAGA Summer SchoolIn order to increase the visibility and attractiveness of IAGA to young researchers, to

motivate them to play active role within IAGA and to create (and enhance) their aware-ness of IAGA and sense of belonging to IAGA, the first IAGA Summer School will be or-ganized just prior the Assembly. The summer school will provide overview of the activities carried out within all the IAGA divisions, with subjects from paleomagnetism and mag-netic anisotropy through observatories and geomagnetic field modeling to ionospheric and aeronomic research. At least 20 young scientists from all around the world will be invited based on the nominations from Working Groups and Divisions. Special call and more information will be published before the end of 2012.

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Description of Symposia

Joint SessionsJ1 Div. I/V Results from SWARM and preceding magnetic satellite missions

After Magsat (1980), Oersted (launched in 1999) and CHAMP (2000-2010), the next satellite mission to provide high-precision measurements of the Earth’s magnetic field is Swarm, an ESA mission due to be launched in the summer of 2012. Swarm will consist of two satellites at an initial altitude of 460-490 km (with orbital inclination of 87,4°) next to each other (allowing measurements of the longitudinal gradient), together with an ad-ditional identical satellite launched (with the same launcher) at a slightly higher initial altitude of 530 km (inclination 88°). All local times are to be explored within the multi-year mission lifetime, with the higher satellite due to progressively shift in local time (by 6 hours after 3 years) with respect to the lower pair of satellites. By the time of this session, Swarm is expected to have been in orbit for about one year, including time for com-missioning, and first data (time series of the magnetic, electric, and acceleration fields together with GPS measurements and orbit determination) should have been released to the scientific community for calibration, validation and first scientific investigations. By then, first results in view of the production of derived data products (by ESA and the in-ternational SCARF facility set up under ESA contract), such as geomagnetic field models for distribution to an even wider public, should also be available.

This session invites all reports on early results and experiences of the Swarm data set, together with reports on progress brought by magnetic data from previous satellite missions, combined with methodological progress, into our understanding of the core, lithosphere, ionosphere, magnetosphere and other minor contributors to the magnetic signal measured in space, such as the electrically conducting mantle and ocean.

Convener: Gauthier Hulot, gh@ipgp.frInstitut de physique du globe de Paris, 4, place Jussieu - Case 89 - 75252 Paris Cedex 05, FrancePhone: +33 (0)1 83 95 74 78

Co-Conveners: Nils Olsen, nio@space.dtu.dkNational Space Institute, Technical University of DenmarkElektrovej Building 327, room 218, 2800 Kgs. Lyngby, DenmarkPhone +45 45259708, Fax +45 45259575Vincent Lesur, vincent.lesur@gfz-potsdam.deGFZ German Research Centre for Geosciences, Section 2.3, Earths Magnetic Field Telegrafenberg, F 453, 14473 Potsdam, Germany Phone: +49 331 288 1271 Fax: +49 331 288 1235

Mexico

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J2 Div. I/VMOD Geomagnetic secular variation and rapid core dynamics from sat-ellite and observatory measurements

In recent years, the combination of globally distributed satellite magnetic data and continuous temporal monitoring by ground magnetic observatories has driven increas-ingly high resolution studies of geomagnetic secular variation. This session focuses on the use of magnetic observations to further improve our understanding of secular variation on time scales of decades and shorter. It will encompass issues of data selec-tion, methods of time-dependent field modelling, and also investigations of the underlying MHD processes in the Earth’s core.

Separation of the core field from other sources (external fields, related induced fields and crustal fields) remains a significant challenge that needs to be better addressed if recent and future magnetic observations are to be fully exploited. Improvements in data error covariance estimates, and new approaches to robust yet physically consistent field modelling are also urgently required. Contributions addressing operational issues re-lated to the IGRF, including how best to construct time-dependent field models in epochs of changing data quality (such as the gap between the low-altitude satellite missions CHAMP and Swarm), and how best to predict future secular variation are particularly encouraged.

On a deeper level, the processes generating secular variation on time scales of dec-ades and shorter (including so-called ‘jerk’ events that may be only a part of a continuous spectrum of rapid variations) remain enigmatic. This session will explore the origin of rapid secular variation, including both the core dynamics and kinematics responsible, the characteristic temporal spectrum and geographical distribution of the rapid secular vari-ation, its relation to torsional oscillations, and its importance for understanding variations in the Earth’s rotation.

Convener: Christopher Finlay, cfinlay@erdw.ethz.chTechnical University of Denmark, National Space InstituteElektrovej, Building 327, 2800 Kgs. LyngbyPhone: +45 45259713

Co-Conveners: Richard Holme, R.T.Holme@liverpool.ac.ukJane Herdman Laboratories, 4 Brownlow Street, L69 3GP, University of Liverpool, United KingdomPhone: +44 (0)151 794 5254, Fax +44 (0)151 794 5196Nicolas Gillet, Nicolas.Gillet@ujf-grenoble.frInstitut des Sciences de la Terre, Université Joseph Fourier 38041 Grenoble CEDEX 9, France Phone: +33 (0)4 76 63 52 65, Fax: +33 (0)4 76 63 52 52

J3 Div. I/V Assimilation of geomagnetic observations in dynamical models of the Earth’s core

Recent years have seen a growing interest in the possibility of applying data assimi-lation techniques to the analysis of geomagnetic observations. Compared with traditional modelling techniques, the novelty here lies in the use of a prognostic numerical model of core dynamics as a source of prior information for the geomagnetic inverse problem. The problem is then to combine this information in an optimal fashion with that contained in the highly heterogeneous observational record, and to modify the trajectory of the dynamical model accordingly. This framework opens the way to new dynamically based methods for retrospective analysis and mapping of past geomagnetic observations, and to improved prospective forecasts of the geomagnetic secular variation.

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This session welcomes contributions covering theoretical, methodological and prac-tical aspects related to this new line of research, e.g., choice of the physical model of core dynamics, choice of prior dynamical error covariances, optimization methods of the assimilation algorithm, and design of operational schemes for the analysis of real data.

Convener: Alexandre Fournier, fournier@ipgp.frInstitut de Physique du Globe de Paris, 1 rue Jussieu , 75238 Paris cedex 05, FrancePhone: (33) 1 83 95 74 75

Co-Convener: Gary Egbert, egbert@coas.oregonstate.eduCollege of Earth, Ocean, and Atmospheric Sciences, Oregon State University 104 CEOAS Administration Building, Corvallis, OR 9, USAPhone: 541-737-2947 Fax: 541-737-2064 7331-5503

J4 Div. I/V Structure, geometries and properties of the continental mantle litho-sphere and asthenosphere constrained by geo- and electromagnetism

The plate tectonic model of the Earth is now over half a century old, and in the main does a reasonable job of describing the surface kinematic movements of the continental and oceanic plates that cover our planet. In the model, the continents comprise thick (60-250 km), buoyant lithosphere riding on more ductile asthenosphere. However, our knowledge of the Earth’s mantle processes and its physical properties in depth is poor to very poor to virtually non-existent. Particularly poorly known are the formation, deforma-tion and destruction processes of the continental lithospheric mantle, and whether these processes evolved through time.This session will bring together IAGA’s geoelectromag-netists and geomagnetists to try to elucidate some of the overarching and outstanding questions in tectonics today concerning the continental mantle lithosphere and astheno-sphere through imaging structures, geometries and properties and drawing inferences and conclusions therefrom.

Convener: Alan G. Jones, alan@cp.dias.ieSchool of Cosmic Physics, Dublin Institute for Advanced Studies 5 Merrion Square, Dublin 2, Ireland Phone: +353-1-653-5147 x224 Fax: +353-1-443-0575

Co-Convener: Erwan Thébault, ethebault@ipgp.frChargé de Recherche CNRS/INSU, Equipe de Géomagnétisme, Institut de Physique du Globe de Paris, Paris Cité 1, rue Jussieu, 75005 Paris Phone: +33 (0)1 83 95 74 84

J5 Div. I/ III Contributions of electromagnetic array studies to understanding solid earth and magnetospheric processes. In memory of Ian Gough

Arrays of magnetometers have been used since the 1960’s to both look up and map spatio-temporal variations in the magnetosphere, and to look down and image the elec-trical conductivity of the Earth for geodynamic studies. Professor Ian Gough played a fundamental role in the early days of these array studies, developing a portable analogue magnetometer that was cheap enough to be produced in large numbers, and then, with colleagues in both the Earth and space sciences, deploying them in large regional arrays. Modern digital instruments, data processing, and numerical modeling methods allow a

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number of new applications. In solid Earth geophysics, arrays of synoptic magnetotel-luric sites (with electric as well as magnetic field measurements) are now often deployed (e.g., the US EMScope, and Chinese Sino-probe MT projects), and interpreted with 3D inversion codes. In solar-terrestrial and magnetospheric physics, ground arrays have provided unique information on meso- and global scales, especially as a complement to and in combination with in-situ satellite measurements (e.g., as a measurement re-quirement for the recent NASA THEMIS mission, and in support of the upcoming NASA Radiation Belt Storm Probes mission to be launched in 2012). Recent advances have also emphasized the capabilities of magnetometer arrays to remote-sense the character of both the solid-Earth and magnetospheric plasma environments through applications of generalized magneto-sounding.

Contributions to a symposium in honor of the memory of Prof. Ian Gough are sought on electromagnetic array studies across the spectrum of Earth and space sciences. Papers focusing on all aspect of magnetometer array studies are welcome, from new instrumentation or data analysis methodologies, to new results about the magnetosphere and solar-terrestrial coupling, or in solid Earth physics. We especially welcome papers which exemplify the scientific value of combining data from multiple arrays (e.g., through InterMagnet or SuperMAG) to study global and mesoscale magnetospheric structure and response to solar wind drivers, or for global studies of mantle conductivity.

Convener: Gary Egbert, egbert@coas.oregonstate.eduCollege of Earth, Ocean, and Atmospheric Sciences, Oregon State University 104 CEOAS Administration Building, Corvallis, OR 9, USAPhone: 541-737-2947 Fax: 541-737-2064 7331-5503

Co-Convener: Ian Mann, imann@ualberta.caDepartment of Physics, 4-181 CCIS, University of Alberta Edmonton Alberta T6G 2E1, CANADA Phone: (780) 492-6882

J6 Div. II/ICMA and CAWSES-II/SCOSTEP Long-term changes and trends in the upper atmosphere-ionosphere system

Long-term changes and trends in the ionosphere, thermosphere, mesosphere and stratosphere are topic of this symposium. Both observational and model investigation pa-pers are welcome. Particular preference will be given to papers which cover more height regions and reveal similarities and dissimilarities between trends at different heights in the atmosphere and uncover origin of such similarities or dissimilarities. Data quality is also a topic as well as the relative role of various trend drivers.

Convener: Gufran Beig, beig@tropmet.res.inIndian Institute of Tropical Meteorology, Physical Meteorology and Aerology Division, Pune, India.

Co-Conveners: Jan Lastovicka, jla@ufa.cas.czInstitute of Atmospheric Physics, Academy of Sciences of the Czech Republic Boční II, 140, 141 31 Prague 4, Czech RepublicPhone: +420 272 764 336, Fax: +420 272 763 745Scott Bailey, scott.m.bailey@vt.edu302 Whittemore Hall, Virginia Tech, Blacksburg, VA 24061 ,USA Phone: +1 540 231 0459 Fax:+1 540 231 3362

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J7 Div. II/III Low Latitude Atmosphere-ionosphere Coupling Processes and Responses to Forcing from Lower Atmosphere and Magnetosphere

The equatorial and low latitude atmosphere-ionosphere system presents unique coupling processes and is subject to drastic modification by dynamical and electro-dy-namical processes arising from upward transport of energy and momentum by gravity-, tidal- and planetary waves originating from lower heights and extra-tropics. As a result large scale zonal, day-to-day and inter-annual variabilities occur in this latitude region. Magnetospheric/interplanetary forcing through disturbance electric fields and energy deposition at high latitudes with coupling to equatorial latitudes represents another im-portant source of variability of the system at different time scales. This symposium will ad-dress all aspects of the dynamics, electrodynamics, energetics and coupling processes of the latitude region extending from the equator to mid-latitudes. Results are welcome from observational (from ground, space, or both), theoretical and modeling investiga-tions. We solicit variety of studies of small and large structures, TEC, winds and waves, temperatures, plasma drifts, electric fields, currents, precursor conditions for equatorial plasma bubble development, anomaly, electrojet variabilities etc., with stress on impor-tance of coupling processes.

Convener: Mamoru Yamamoto, yamamoto@rish.kyoto-u.ac.jpResearch Institute for Sustainable Humanosphere (RISH), Department of Communications and Computer Engineering, Kyoto University Gokasho, Uji, Kyoto 611-0011, Japan Phone: +81-774-38-3814, Fax: +81-774-31-8463

Co-Convener: Mangalathayil A. Abdu, maabdu@dae.inpe.brINPE Divisao de Aeronomia, Av. dos Astronautas 1578 Sao Jose dos Campos SP 12245-970, Brazil Phone: +55-12-2945-7149, Fax: +55-12-3945-6990

J8 Div. II/III Extreme Space Weather: Solar wind-magnetosphere-ionosphere-upper atmosphere coupling

The extremes of space weather are interesting because such extremes provide us with valuable information about the physical processes involved in the coupled Sun-Earth system, and their effects on technology and climate. The session will provide a forum to discuss the extreme space weather phenomena and processes such as the origin and propagation of CMEs and ICMEs, solar wind-magnetosphere interactions, auroral processes, geomagnetic storms and sub-storms, ionospheric storms and thermospheric storms, and events during the recent deep extended solar minimum. The space weather effects on satellite systems, power supply systems and Earth’s climate are of particular interest. Papers dealing with observations, theory and modeling of the extreme space weather phenomena and coupling processes on global and regional scales are solicited.

Convener: Nanan Balan, b.nanan@sheffield.ac.ukDepartment of Automatic Control and Systems Engineering, University of Sheffield, Sheffield S1 3JDPhone: (+44) (0)114 222 5234, Fax: (+44) (0)114 222 5683

Co-Conveners: Tiger Liu, tigerjyliu@gmail.comDepartment of Earth Sciences, National Central University, No.1, University Road, Tainan City 701, Taiwan (R.O.C.)Phone: (886)-6-275-7575

Andrew Yau, yau@phys.ucalgary.caPhysics and Astronomy, University of Calgary, 2500 University Dr. NW

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Calgary, Alberta, Canada, T2N 1N4Phone: +1(403)220-8825

J10 Div. II/III/ICMA Energetic particle precipitation into the atmosphere: sources and consequences

Particle precipitation into the atmosphere is one of the mechanisms for energetic electron loss from the Van Allen radiation belts. This is particularly significant during and after geomagnetic storms, when the loss rate, and the source population, can both increase. This session is targeted at both ground-based and satellite experimental obser-vations, as well as theoretical investigations, into the precipitation of energetic electrons (>20 keV) into the D-region ionosphere and below. Papers considering the precipitation drivers, the nature of the particle fluxes, or the impact of the precipitation on the iono-sphere or atmosphere are welcome. We particularly welcome early results from RBSP, showing energetic electron loss examples and processes and how it can be applied by the atmospheric community.

Convener: Craig J. Rodger, crodger@physics.otago.ac.nzDepartment of Physics, University of Otago, 730 Cumberland St, Dunedin 9016. New ZealandPhone: (03) 479 4120

Co-Conveners: Mark Clilverd, macl@bas.ac.ukBritish Antarctic Survey, High Cross, Madingley Road, Cambridge CB3 0ET, United Kingdom

Marianne Daae, marianne.daae@ntnu.noNorwegian University of Science and Technology7491, Trondheim, Norway Phone: +47 73591861

J11 Div. II/III The Earth’s Plasmasphere: Modelling and Remote Sensing

The dynamics of the plasmasphere plays an important role in Earth’s space weather system, and is governed by solar activity. Also the plasmasphere is strongly coupled to the ionosphere by means of electromagnetic fields and currents. The plasmasphere forms the cold plasma background for the overlapping ‘warm’ (ring current) and ‘hot’ (radiation belts) regions and its plasma distribution is a fundamental parameter for the description and modelling of various physical processes in these regions. This session focuses on various remote-sensing techniques: active and passive ground-based meas-urements using ULF-ELF-VLF electromagnetic waves as well as satellite-based methods including radio sounding and imaging. Also included are the coupling processes related to cold plasma density.

Convener: Fred Menk, Fred.Menk@newcastle.edu.auSchool of Mathematical and Physical Sciences, The University of Newcastle, University Drive, Callaghan, NSW 2308, AustraliaPhone (02) 4921 2005, Fax (02) 4921 7949

Co-Conveners: Lános Lichtenberger, lityi@sas.elte.hu Pontus Brandt, Pontus.Brandt@jhuapl.edu

Applied Physics Laboratory, Johns Hopkins University, 7-336 11100 Johns Hopkins Road, Laurel,. MD 20723

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Second circular

J13 Div. IV/ III/ II From micro- to macro-scales in the heliosphere and magnetospheres

The sun emits a continuous stream of charged particles, known as the solar wind (SW), which expands and displaces the partially ionized interstellar gas to form the he-liosphere. Inside the termination shock (TS) the supersonic SW interacts with planetary magnetic fields to produce localized planetary plasma environments known as magne-tospheres. Macroscopically, magnetospheres and the heliosphere have similar qualita-tive structural aspects: bow shock, plasma-pause, plasma sheath, plasma tail. At each of these plasma structures, similar microphysics comes into play: particle acceleration, wave-particle interactions, shock microphysics, reconnection. In this session we seek contributions that investigate the structure of the heliosphere and/or the magnetosphere at different scales, and especially contributions that highlight similarities and differences between the two types of structures.

Convener: Igor Veselovsky, veselov@dec1.sinp.msu.ruSkobeltsyn Institute of Nuclear Physics, Moscow State University, 119234 Moscow RussiaPhone: +7(495)939-1298, Fax: +7(495)939-3553

Co-Convener: Jacob Heerikhuisen, jh0004@uah.eduThe University of Alabama in Huntsville, 301 Sparkman Drive Huntsville, Huntsville, AL 35899, USA Phone: 256-961-7403, Fax: 256-961-7730

J14 Div. IV/II/III Heliospheric structure during the ascending phase of solar cycle 24

As solar activity increases during the ascending phase of the solar cycle the he-liosphere becomes highly perturbed by large scale structures (coronal mass ejections, corotating interaction regions, interplanetary shocks). This session welcomes studies related to these structures based on combined observations (white light, radio, IPS, in situ), as well as contributions based on simulation results. Our goal is to understand in more detail the changes that the 3-D heliosphere suffers as solar wind and large scale structures change towards solar maximum.

Convener: Xochitl Blanco-Cano, xbc@geofisica.unam.mx Instituto de Geofísica, UNAM. Circuito de la investigación Científica s/n, Ciudad Universitaria, Delegación Coyoacán, C.P. 04510, México D.F., Mexico

Co-Convener: Lan K. Jian, jlan@igpp.ucla.eduInstitute of Geophysics and Planetary Physics, UCLA, 3845 Slichter Hall, 603 Charles E. Young Drive, East, Los Angeles, CA 90095-1567 Phone: 310-206-2285

J15 Div. III/ IV Plasma interactions at solar system bodies without or with weak intrinsic magnetic field

This session will be a forum for presenting recent progress in the space plasma phys-ics of solar system bodies without or with weak intrinsic magnetic field. The interaction of Mars and Venus with the solar wind is mainly of the atmospheric type, at comets a comparable situation is met. At Mercury with its only weak intrinsic field, parts of the exo-sphere are exposed to the solar wind leading to similar atmospheric effects. Interaction of the weakly magnetised Earth Moon or of non-magnetic satellite bodies with the local

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plasma environment of their planet shows different aspects of a similar process. The session welcomes recent results from Mars, Venus and Mercury missions, from Cassini around Saturn’s moons and to results from the Kaguya (Selene) mission to the Earth Moon. Presentation of new results from a combined analysis of data from different instru-ments as well as from comparison of different planets and satellites is encouraged. Open topics on plasma boundaries and their dynamics, atmospheric and ionospheric escape, upstream waves, etc. will be discussed.

Papers on numerical simulation, theoretical studies and comparison of numerical or theoretical results with recent data analysis are highly welcomed, as well as studies fo-cussing on upcoming space missions like Bepi-Colombo to Mercury and Rosetta’s arrival at Comet Churyumov-Gerasimenko.

Convener: Magda Delva , magda.delva@oeaw.ac.atÖsterreichische Akademie der Wissenschaften, Institut für Weltraumforschung Schmiedlstraße 6, 8042 Graz, Austria Phone: +43 (316) 4120-400, Fax: +43 (316) 4120-490

Co-Conveners: Christian Mazelle, christian.mazelle@cesr.fr CESR, 9, avenue du Colonel Roche, F-31400. Toulouse Cedex,France, Phone: +33 5 61 55 66 50

Cesar Bertucci, cbertucci@iafe.uba.arInstitute for Astronomy and Space Physics (IAFE), Buenos Aires, Argentina, Phone: +54 11 47868114),

Naoki Terada, teradan@stpp.gp.tohoku.ac.jpSpace and Terrestrial Plasma Physics Laboratory, Department of Geophysics, Tohoku University, 6-3,Aramaki Aza-Aoba,Aoba-ku,Sendai 980-8578, Tohoku, JapanPhone: +81-22-795-6515

J16 Div. III/IDCH History of Research on the Radiation Belts

In 1958 James Van Allen and co-workers discovered the Earth’s radiation belts using a simple Geiger counter. In the more than 30 years since that seminal observation, our understanding of the Earth’s radiation belts has changed dramatically and new questions about the fundamental processes of energetic particle acceleration, transport, and scat-tering have emerged. This session focuses on the critical discoveries and missions that have shaped our understanding of radiation belt physics. We will examine how particular space weather events (e.g. March 1991 and January 1997 and others), fundamentally altered the course of radiation belt research. Similarly long-term, climatological, obser-vations now span several solar cycles providing new understanding of variability and context for individual events. We will consider the missions that revolutionized our un-derstanding of radiation belt dynamics (e.g. CRRES, POLAR, SAMPEX and others) and what unique aspects of those observations shaped new paradigms. The “Radiation Belt Revolution” of the 1990s provided the motivation and impetus for a new generation of radiation belt missions including Radiation Belt Storm Probes (RBSP), the Energization and Radiation in Geospace (ERG) mission, Resonance, and others. This session will also discuss new radiation belt observations that hold promise for solving long-standing problems and the emergence of new paradigms for understanding radiation belt accel-eration, transport, and loss.

Convener: Geoffrey D. Reeves, reeves@lanl.govLos Alamos National Laboratory, Mail Stop D466

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Second circular

Space Science & Applications, Los Alamos, NM 87545-0000, USAPhone: (505)665-3877 Fax: (505)665-7395

J17 Div. II/IDCH History of Ionosonde Research

The ionosonde have been the work horse of ionospheric research for many decades. From the discovery of the ionospheric layers and their diurnal and seasonal variations to ionospheric dynamics and spread F, ionosondes have provided the basic measure-ments. Over time the ionosonde itself underwent a steady development from a relatively simple analog instrument to a highly sophisticated digital radar system, and the initial ground-based observations extended to satellite borne topside observations. We solicit papers on significant ionospheric research with ionosondes from ground and satellites and on the development of ionospheric sounders.

Convener: Bodo W. Reinisch, Bodo.Reinisch@Digisonde.comLowell Digisonde International, LLC, 175 Cabot Street, Suite 200, Lowell, MA 01854, USAPhone: +1 978.735.4752, Fax +1 978.735.4754

Co-Conveners: Mangalathayil Abdu, abdu.manga@gmail.comINPE Divisao de Aeronomia, Av. dos Astronautas 1578 Sao Jose dos Campos SP 12245-970, BrazilTel: +55-12-2945-7149 Fax: +55-12-3945-6990

Gordon James, gordon.james@crc.gc.caCommunications Research Centre Canada, 3701 Carling Avenue, P.O. Box 11490, Station “H”, Ottawa, Ontario K2H 8S2, CanadaPhone: +1 613 998 2230, Fax: +1 613 990 6339

J18 ICDC Div. II / III / V Characterization of Ionospheric and Magnetospheric Processes from ground and satellite observations

This session will accept contributions for both oral and poster presentations on gen-eral studies of the ionosphere and magnetosphere. The emphasis will be on the char-acterization of ionospheric and magnetospheric processes using ground and/or satellite observations, but theoretical and simulation studies are also welcome. Special emphasis will be given to the relevance of those studies to developing countries.

Convener: Inez Batista, inez@dae.inpe.brNational Institute for Space Research (INPE), Av. dos Astronautas, 1758 12227-010 São José dos Campos, SP, BrazilPhone: +55 12 3208 7153, Fax: +55 12 3208 6990

Co-Conveners: Pieter Kotze, pkotze@sansa.org.zaHermanus Magnetic Observatory, PO Box 32, Hermanus 7200, South Africa Phone: +227 283 21196

K. Veera Swamy, kv.swamy@gmail.comNational Geophysical Research Institute, Uppal Road, Hyderabad - 500 007, A.P. India Phone: +91 40 23434771

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Division 1 1.1 Planetary dynamos and core dynamics

The last decade has yielded significant improvements in models of the dynamics of planetary cores. Numerical dynamo simulations have been used to investigate fluid mechanical and magnetohydrodynamic processes in a range of astrophysical bodies at different stages of their evolution using a variety of driving mechanisms, and control pa-rameters. The development of scaling laws and the use of powerful computers to inves-tigate the rapidly rotating regime characteristic of many planetary cores have facilitated comparisons between these simulations and the growing body of observational data. Moreover, continued improvements in understanding of the couplings between planetary cores and the solid or fluid shells that enclose them have provided new avenues for investigating core processes. This session invites general contributions relevant to the dynamics of planetary cores.

Convener: Mathieu Dumberry, dumberry@ualberta.caUniversity of Alberta Edmonton, AB, T6G 2E1 Canada.Office: CCIS 3-093. Phone: +1-780-492-3987. Fax:+1-780-492-0714

Co-Convener: Chris Davies, c.davies@leeds.ac.ukUniversity of Leeds School of Earth and Environment Leeds, LS2 9JT United Kingdom Phone: +44 (0) 11 33 43 55 43

1.2 Experimental MHD and hydrodynamic processes

There is growing interest in understanding MHD processes through direct experi-ment. The last decade has seen some exciting results concerning magnetic field gen-eration in electrically conducting fluid media and hydrodynamic processes in buoyancy drive and boundary driven flows. Examples of analogue experiments stretch from those concerned with tides, precession and libration through to rapidly rotating experimental dynamos. A range of instabilities has been studied, from boundary layer problems to the Magnetorotational instability (MRI). Furthermore, as strong magnetic fields have become more easily available, it has become an opportunity to study Alfven waves in the labora-tory. Much remains to be understood, not least the effects of turbulence, modified by magnetic and rotational forces. Studies of weak turbulence, dominated by linear waves (inertial, Rossby, Alfven, torsional) at short time-scale, are highly relevant and appropri-ate. We solicit submissions concerned with experiments aimed at understanding plan-etary fluid dynamical phenomena, in all types of fluid and plasma. Our session welcomes all submissions concerned with experiments, including associated theory and numerical simulation papers.

Convener: Andrew Jackson andrew.jackson@erdw.ethz.chETH Zürich, Institut für GeophysikSonneggstrasse 5, CH-8092 Zürich, SwitzerlandPhone: +41 44 633 7349 (work) +41 43 288 5369 (home)

Co-Convener: Thierry Alboussiere thierry.alboussiere@ens-lyon.frGeophysics department, University of Lyon, ENS-Lyon, FrancePhone: (33) 4 72 44 83 9

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Second circular

1.3 Electromagnetic imaging of crustal structures and processes

Electromagnetic method can image the distribution of resistivity which is sensitive to existence and connectivity of minor but important constituents of the crust, such as conducting minerals, graphite, partial melts, and fluids, which will constrain the tectonic processes. This session welcomes crustal imaging studies in Archaean cratons to recent active tectonic zones. Comparisons with other geophysical data from seismology and geodesy, or with geochemical data are very much encouraged.

Convener: K. Veera Swamy, kv.swamy@gmail.comNational Geophysical Research Institute, Uppal Road, Hyderabad - 500 007, A.P. India Phone: +91 40 23434771

Co-Conveners: Jorge Arzate, arzatej@geociencias.unam.mxCentro de Geociencias, Universidad Nacional Autónoma de México (UNAM), Blvd. Juriquilla No. 3001, Querétaro, 76230, MéxicoPhone: +52 442 238 1104, ext. 111

Yasuo Ogawa, oga@ksvo.titech.ac.jpTokyo Institute of Technology, i6-34 (titech postal code), 2-12-1 Ookayama, Meguro, Tokyo, 152-8551, JapanPhone: +81-3-5734-2639 Fax.+81-3-5734-2492

1.4 Near surface application of electromagnetic induction

Electromagnetic geophysical methods have been applied in mapping the electri-cal conductivity structure of the ground, particularly for near-surface investigations. Examples include contaminated unconfined aquifers associated with landfills, landslides, seawater intrusion in coastal areas, the detection of cavities, and the detection of sink-holes, caves in karstic areas, mineral exploration as well as archaeological studies. With the development of new technologies, new instruments, and improved data-processing, electromagnetic methods are able to image shallow structures with applications to many environmental and near surface problems. We would like to invite contributions related to the issues mentioned above, including case studies, the development of novel applica-tions of electromagnetic methods, and the joint inversion of electromagnetic data with other geophysical datasets.

Convener: Gad El-Qady gadosan@nriag.sci.eg, gadosan@yahoo.com National Research Institute of Astronomy and Geophysics (NRIAG), P. O. Box: 227, Helwan, 11722, Cairo, Egypt

Co-Convener: Mark Everett, mark.e.everett@gmail.comDepartment of Geology and Geophysics, MS 3115, Texas A&M University,College Station, Texas 77843-3115, USA Phone: 979.862.2129, Fax: 979.845.6162

1.5 Advances in electromagnetic modelling and inversion

The accurate prediction of galvanic distortions, both electric and magnetic, of in-creasingly detailed land, marine and airborne surveys as well as their interpretation in terms of realistic models of underground targets (from small UXO to large mantle struc-tures), require a continuous evolution of electromagnetic modelling and inversion strate-gies of all kinds of electromagnetic data. With two-dimensional modelling well developed,

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there is the challenge of revisiting model propositions and uncertainty evaluation, with topics such as the assimilation of multicomponent data and prediction of electrical ani-sotropy. There is also an increased need to improve three dimensional modelling strate-gies for multisource data such as AEM and Marine CSEM, with their optimization and massive parallel computation challenges, as well as the need to evaluate the feasibility of time lapse EM modelling and inversion for water and hydrocarbon reservoirs. The combination of various types of EM and other geophysical data in joint inversion is also a field of much scientific and industry attention. In this session we invite contributions on recent developments on modelling and inversion of the several types of EM data in all dimensionality contexts and in combinations with other geophysical data. Cases history of the application and uncertainty evaluation of well established and emerging modelling strategies are also welcome for this session.

Convener: Luis A. Gallardo, lgallard@cicese.mx Department of Applied Geophysics, CICESE, Carretera Ensenada-Tijuana No. 3918, Zona Playitas, C.P. 22860, Ensenada, B.C., MexicoPhone: +52 646 1750500 Ext. 26320, Fax +52 646 1750567

Co-Convener: Enrique Gómez-Treviño, egomez@cicese.mxDepartment of Applied Geophysics, CICESE, Carretera Ensenada-Tijuana No. 3918, Zona Playitas, C.P. 22860, Ensenada, B.C., MexicoPhone:+52 646 1750500 Ext. 26313, Fax +52 646 1750567

1.6 Marine electromagnetic studies

EM community members interested in marine electromagnetics are invited to submit papers to the session “Marine electromagnetic studies” for the IAGA 2013 12th Scientific Assembly, to be held from August 26 to 31, 2013, in Mérida, Yuc., Mexico.

Marine geophysical exploration using electromagnetic techniques has been a subject of explosive evolution during the last decade. In this fast-developing science, unprec-edented achievements parallel new open questions and challenges. We invite contribu-tions in natural and controlled source marine EM, including advances in measurement techniques and instrumentation, data processing and analysis, as well as case histories from academics and industry.

Convener: José M. Romo, jromo@cicese.mxDepartment of Applied Geophysics, CICESE, Carretera Ensenada-Tijuana No. 3918, Zona Playitas, C.P. 22860, Ensenada, B.C., MexicoPhone:+52 646 1750500 Ext. 26311, Fax, +52 646 1750567

Co-Convener: Steven Constable, sconstable@ucsd.eduScripps Institution of Oceanography, 8800 Biological Grade, La Jolla CA 92093-0225, USA Phone: 1-858-5342409, Fax: 1-858-5348090

1.7 Time variability of the geomagnetic field: supechrons, reversals, secular caria-tion, jerks

The time spectrum of the geomagnetic field encompasses a wide range of time-scales. This is being revealed in new detail by paleomagnetic data from lava and sedi-mentary rocks, archeomagnetic data, and historical records. We encourage contributions reporting on these data and on their analysis and interpretation in terms of the Earth’s internal dynamo.

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Convener: Fabio Donadini, fabio.donadini@gmail.com Institut für Geophysik, ETH Zürich, Sonneggstrasse 5, 8092 Zürich Phone: +41 44 632 3980

Co-Conveners: E. Joshua Rigler, erigler@usgs.gov USGS Golden, Box 25046, MS966, DFC, Denver CO 80225, USA Phone: 303-273-8607, Fax 303-273-8600

Joseph Liddicoat, jliddico@barnard.edu Barnard College, 3009 Broadway, New York, NY 10025-6598, USA Phone/fax: (212) 854 7089/5760

Hatem Odah, hatemodah@yahoo.com National Research Institute of Astronomy, and Geophysics, 11277, Helwan, Egypt.Phone+ 202 25541100, Fax: + 202 25548020

1.8 Paleomagnetism and dating

The usefulness of the geomagnetic polarity timescale (GPTS) depends crucially on the precision of its correlation to absolute ages (dating), but also to the precision of corre-lation to other facets of geologic time such as marine isotopic stages and biostratigraphic zonations. Global manifestation and synchroneity of polarity reversals have made the polarity record central to geologic timescales over the last ~160 Myrs, and have ac-centuated the importance of these correlations. As precision in stratigraphic correlation becomes more important for understanding leads and lags in the paleoclimate record, the use for correlation of within polarity-chron paleomagnetic records, such as directional secular variation, magnetic excursions, and relative paleointensity (RPI), has become more widespread but over what spatial and temporal timescales can they be useful? Precision and accuracy in correlation and dating depends on the type of record (e.g. sed-imentary, extrusive, archeological artefact), and ranges from years for historical secular variation records to tens of years for archeomagnetic observations, and up to thousands of year for older records of RPI, excursions, and reversals. We solicit contributions that deal with dating and correlating records of secular and archeomagnetic variations, RPI, excursions, and polarity reversals, using different dating and correlation methods.

Convener: Luis Alva-Valdivia, lalva@geofisica.unam.mxInstituto de Geofisica, UNAM, Ciudad Universitaria, Mexico-City 04510, MéxicoPhone +52-55-56224237

Co-Conveners: Cor Langereis, langer@geo.uu.nlPaleomagnetic Laboratory ‘Fort Hoofddijk’, Department of Earth Sciences, Utrecht University, Budapestlaan 17, 3584 CD Utrecht, The Netherlands (+31.30.253.1668)

Jim Channell, jetc@ufl.eduDepartment of Geological Sciences, 241 WIlliamson Hall , P.O. Box 112120, Gainesville, FL 32611-212, USA.Phone: (352) 392-3658

1.9 Paleomagnetic reference models (GPTS, APWP, etc)

The paleomagnetic field has provided temporal and spatial frameworks which have been applied in a variety of stratigraphic, tectonic, paleogeographic and geodynamic

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problems. Examples of such models include apparent polar wander paths for continents and oceans, marine magnetic anomaly models and the geomagnetic polarity time scale. In many aspects, some of those models provide insufficient resolution to treat long stand-ing questions such as true polar wander, uncertainties in hot spot reconstructions and long-term stability of the deep mantle and outer core.

APWP´s are also in dire need of reconsideration in the context of remanence acquisition artifacts, improved dating techniques and long-term non-dipole field behavior. This session thus invites contributions from all fields of paleomagnetism and geomagnetism related to temporal and spatial reference models and their application in the earth sciences.

Convener: Roberto Molina, rmolina@geociencias.unam.mxCentro de Geociencias, Universidad Nacional Autónoma de México, Blvd. Juriquilla No. 3001, Querétaro, 76230, MexicoPhone: +52 442 238 1104, ext. 126

Co-Conveners: Jenny Tait. jenny.tait@ed.ac.ukSchool of GeoSciences, The University of Edinburgh, Grant Institute, The King’s BuildingsWest Mains Road, Edinburgh EH9 3JWPhone: +44 (0) 131 651 7069, Fax: +44 (0) 131 668 3184

Baochun Huang, bchuang@mail.iggcas.ac.cnInstitute of geology and Geophysics, Chinese Academy of Sciences, No. 19, Beitucheng Western Road, Chaoyang District, 100029, Beijing, China.P.R.Phone: 010-82998001, Fax 010-62010846

1.10 Paleomagnetism and magnetic fabrics applied to tectonic processes

The following session aims to summarize the latest findings in the field of paleomag-netic analysis together with magnetic fabrics and their application to tectonic processes. Contributions dealing with the combination of anisotropy of magnetic susceptibility ac-quired in both low and high fields as well as anisotropy of remanent magnetizations with classical paleomagnetic studies are welcome. Topics for this session include, but are not restricted to, new traditional paleomagnetic results from rocks of all ages applied to tec-tonic processes, magnetic stratigraphy of sedimentary basins, magnetic fabrics studies in metamorphic terrains and igneous complexes, magnetic fabrics and other methods to correct paleomagnetic directional data (i.e. inclination shallowing), new techniques of magnetic fabrics analysis and/or fabrics separation, measurements of magnetic fabrics at different applied low-fields and interpretation of remanence fabrics, and non-traditional applications of magnetic fabrics. Special attention will be paid to the studies that combine magnetic methodologies with others such as microstructural analyses, field observations, and their different scales of application. The session integrates also other research lines within the field of magnetic fabrics such as time and processes of lock in of the magnetic anisotropies in recent sediments, from both marine and terrestrial environments.

Convener: Satria Bijaksana, satria@fi.itb.ac.idFaculty of Mining and Petroleum Engineering, Institut Teknologi Bandung, Jalan Ganesa 10, Bandung 40132, Indonesia.

Co-Conveners: Augusto Rapalini, rapalini@gl.fcen.uba.arInstituto de Geofísica Daniel Valencio, Universidad de Buenos Aires, Pabellón 2, Ciudad Universitaria, C1428EHA Buenos Aires, Argentina

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Fatima Martin Hernandez, fatima@fis.ucm.esFacultad de Ciencias Físicas, Ciudad Universitaria s/nUniversidad Complutense de Madrid, 28040 MADRID, SpainPhone: 91-394.51.90, Fax: 91-394.43.98

Irene Raposo, irene@usp.brInstituto Astronômico e Geofísico, Universidade de São Paulo, C.P. 9638, 01065-970 São Paulo, Brazil.

1.11 Open session on paleomagnetism and rock magnetism

This session provides the opportunity for contributions that fall within the broad spec-trum of Paleomagnetism and Rock magnetism but are not directly appropriate to any of the other proposed sessions. We welcome contributions on magnetic studies of different past and present environments, as well as on new methods and developments of labora-tory and field experiments, data analysis and interpretation. Multi-disciplinary approaches involving other complementary physical and chemical methods in addition to palaeomag-netic and rock magnetism studies are highly encouraged. We expect presentations on novel theoretical and experimental concepts and provocative theories in order to stimu-late discussions and exchange of ideas among the authors and audience.

Convener: Mili Aldana, maldana@usb.veDepartamento de Ciencias de la Tierra, Universidad Simón Bolívar, Edif. FE2, Ofic. 312, Sartenejas, Baruta, Edo. Miranda, Venezuela, 1080-A Apartado postal 89000. Phone:+58-212-9063516, Fax:+58-212-9063503.

Co-conveners: Elina Aidona, aidona@geo.auth.grDepartment of Geophysics, School of Geology, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece

Chunxia Zhang, cxzhang@mail.iggcas.ac.cnPaleomagnetism and Geochronology Lab, State Key Laboratory of Lithospheric Evolution, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029, China

1.12 Applied Rock Magnetism: Toward a better understanding of controlling fac-tors of environmental magnetic proxies

Environmental magnetism was established in the 1980’s as a new field and has been thriving for nearly thirty years. Magnetic properties of rocks and minerals are increasingly and widely applied to track sedimentary processes, decipher environmental changes, and reconstruct climatic histories from various sedimentary archives including marine, fluvial-lacustrine, and windblown deposits. Magnetic proxies for environmental and pale-oclimate changes are appealing because most measurements are non-destructive, fast, and can be applied to large sample sets. However, when compared to other proxies, rock-magnetic paleoclimate reconstructions are seldom quantitative, and often the pro-cesses that link past environmental signals to the observed magnetic parameters in sedi-ments or soils are poorly understood. To enhance the applications of environmental mag-netism in geological and environmental studies, this session invites contributions that fall within the broad field of environmental magnetism. Contributions that clarify and quantify factors that determine sediment magnetic signals and link them to past environments via field investigations, theoretical models, magnetic instrumentation, and interdisciplinary parameter comparisons are particularly welcome.

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Conveners: Yongxiang Li, frankyxl@gmail.comState Key Laboratory for Mineral Deposits Research, Department of Earth Sciences, Nanjing University, Nanjing 210093, China

Julie Carlut, carlut@ipgp.fr Géosciences Marines, Cuvier, IPGP - 1 rue Jussieu - 75252 Paris cedex 05; FrancePhone: 01 83 95 76 68

Co-Conveners: Qingsong Liu, liux0272@yahoo.comInstitute of Geology and Geophysics Academy of Sciences (IGGCAS), No. 19, Beitucheng Western Road, Chaoyang District, 100029, Beijing, China.P.R.Phone: 010-82998001, Fax 010-62010846

Junsheng Nie, niejunsheng@gmail.comKey Laboratory of Western China’s Environment System, Ministry of Education, Lanzhou University, 222 Tianshui South Road, Lanzhou, Gansu 730000, China

1.13 Theoretical and Experimental Rock Magnetism

Theoretical magnetism is the cornerstone of all rock and paleomagnetic methods and is fundamental to our understanding of natural systems. This session brings together a broad range of advances in theoretical magnetism including experimental or analytical methods, development of our knowledge of fundamental rock magnetic properties, and proof-of-concept studies linking magnetic properties to natural processes using control experiments. We welcome and encourage contributions focusing on fundamental rock magnetism, numerical modeling of magnetic phenomena, magnetic behavior of nanopar-ticle systems, magnetotactic bacteria, ultrafine particulate matter (PM2.5). Theoretical and experimental studies aimed at resolving open questions, such as accurate and ef-ficient paleointensity determination, the origin of magnetic anisotropy in ferromagnetic particles, and lock-in mechanisms during acquisition of magnetization, etc., will complete the scope of the session. We aim to attract contributions where well-characterized sam-ples (synthetic or natural) are used to investigate fundamental magnetic behaviour or demonstrate the validity of new methods.

Convener: Greig Paterson, greig.paterson@googlemail.comPaleomagnetism and Geochronology Laboratory, Institute of Geology and Geophysics, Chinese Academy of Sciences, Room 418, New Building, 19 Bei Tu Cheng Xi Lu Road, Beijing, 100029, China

Co-Conveners: Neli Jordanova, vanedi@geophys.bas.bgNational Institute of Geophysics, Geodesy and Geography, BA, Acad. G. Bonchev Str., bl.3 1113 Sofia, Bulgaria

Aleksey Smirnov, asmirnov@mtu.eduDepartment of Geological and Mining Engineering and Sciences, Michigan Technological University ,630 Dow ESE Building, 1400 Townsend Drive, Houghton, MI 49931, USAPhone: (906) 487-2365, Fax: (906) 487-3371

Joshua Feinberg, feinberg@umn.eduDept. of Earth Sciences, University of Minnesota, 310 Pillsbury Drive S.E. Minneapolis, MN 55455-0219, USAPhone: 612 624-8429, 612 626-4331

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Division 2 2.1 Equatorial spread-F and F3-layer studies during geomagnetic quiet and dis-

turbed periods

The occurrence of equatorial spread-F and the development of the F3-layer present a strong day-to-day variability, mainly caused by the thermospheric wind and wave ac-tions (gravity waves, tides, planetary waves, TIDs and MSTIDs). Recent multi-instrument and multi-site observations, as well as, theoretical and simulation investigations have advanced our understanding of these phenomena, both during geomagnetic quiet and disturbed periods. The objective of this symposium is to bring together experimentalists and theoreticians to survey the latest results, examine new ideas and concepts, and to indicate important future directions in equatorial and low-latitude research.

Convener: Paulo R. Fagundes, fagundes@univap.brUniversidade do Vale do Paraiba, Av Shishima Hifumi 2911, Sao Jose dos Campos, SP 12244-000, BrazilPhone: +55 12 39471130, Fax +55 12 39471149

Co-Convener: Jonathan J. Makela, jmakela@illinois.edu316 Coordinated Science Lab, MC 228 1308 W. Main St. Urbana, Illinois 61801, USA.Phone: +1 217 265 9470, Fax +1 217 333 4303

2.2 Div II/ICMA Electrodynamics and energetics of the middle atmosphere and lower thermosphere: the local and global picture The wide range of interest in the mesosphere and lower thermosphere has been

recently fuelled by dedicated satellites and new ground-based instruments designed to enhance our understanding of the coupling and energy transfer between the Earth’s at-mosphere and near Earth-space. Effects induced by internal and external sources, such as the impact of lightning discharges, up- and downward streaming energetic charged particles and their hard radiation, cosmic rays, atmospheric waves, meteors and novel radio remote sensing strategies are considered. Localized, inter-hemispheric and global effects are of interest.

Convener: Franz-Josef Luebken, luebken@iap-kborn.deLeibniz-Institut für Atmosphärenphysik e.V. an der Universität Rostock Schlossstraße 6, 18225 Kühlungsborn, GermanyTel. +49 (0) 38293 68 100, Fax +49 (0) 38293 68 50

Co-Conveners: Craig Rodger, crodger@physics.otago.ac.nzDepartment of Physics, University of Otago, PO Box 56, Dunedin 9016NEW ZEALAND Phone: +64 3 479 4120, Fax: +64 3 479 0964

Richard Goldberg, richard.a.goldberg@nasa.govNASA/GSFC, Mail Code: 674, Greenbelt, MD 20771, USAPhone 301.286.8603, Fax 301.286.1648

Martin Fullekrug, eesmf@bath.ac.ukDept. of Electronic and Electrical Engineering, Centre for Space, Atmospheric and Oceanic Science, University of Bath, Bath, BA2 7AY , United Kingdom Phone: +44 (0) 1225 386053

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2.3 Div II/ICMA Coupling Processes in the Atmosphere-Ionosphere System

The Earth’s atmospheric regions are intricately coupled to one another via various dynamical, chemical, and electrodynamic processes. However, the manner in which the couplings take place due to varying energy inputs from the Sun and from the lower atmos-phere is a question that is yet to be understood. The coupled effects can be in terms of the modulation of waves from lower to upper atmosphere as well as from low to high latitudes, electrodynamic and compositional changes, and plasma irregularities at different latitudinal regions of the globe due to the varying energy inputs. The MLT region is a critical region in the coupling between the lower/middle atmosphere and the upper atmosphere/ionosphere since it is here that physical processes filter and shape the flux of waves ascending through the mesosphere into the overlying thermosphere. On the other hand it is reasonable to presume that there might be a link between solar variability and the changes in the middle atmosphere and climate variables. This requires much improved knowledge and under-standing of the solar effects on the coupling processes.

This symposium solicits papers dealing with experiments, observations, modeling and data analysis that describe the effects of atmospheric coupling processes within the atmosphere-ionosphere system. It will address both theoretical and empirical recent results concerning the coupling mechanisms through dynamics, composition and elec-trodynamics. The symposium will be particularly focused on the dependence of coupling processes on the solar and geomagnetic activity, the downward control effects transfer-ring from the strongly solar dependent structure to the lower atmospheric levels.

Convener: Dora Pancheva, dpancheva@geophys.bas.bgGeophysical institute: Acad G. Bonchev Str. Block 3, 1113 Sofia, BulgariaPhone: + 3592 971 3308, Fax: + 3592 971 3005

Co-Conveners: Ulrike Langematz, ulrike.langematz@met.fu-berlin.deInstitut für Meteorlogie, Carl-Heinrich-Becker-Weg 6-10, 12165 Berlin, GermanyPhone: +49 30 838 71 165, Fax: +49 30 838 71 128

Petra Knizova, pkn@ufa.cas.czInstitute of Atmospheric Physics, Czech Academy of Sciences Boční II, 1401 141 31 Prague 4, Czech RepublicPhone: +420 272 764 336, Fax: +420 272 763 745

2.4 Div II/ICMA and CAWSES-II/SCOSTEP Long- and short-term solar influences in the middle and upper atmosphere

With increasing altitude solar variability becomes the dominant forcing mechanism for atmospheric and ionospheric variability at time scales from hours to decades. However, forcing from below essentially through waves (gravity waves, tides, planetary waves) has been detected as well. From available datasets it is not always straightforward to distinguish between solar and meteorological influences. Time series are often too short to clearly identify, e.g., the 11-year solar cycle in the presence of nonlinear trends owing to lower atmospheric variability. The effect of planetary waves at time scales of days to weeks is difficult to extract from time series in the presence of the solar rotation effect and harmonics. Furthermore, open questions remain about the propagation mechanism especially of planetary waves to the mesosphere/thermosphere/ionosphere.

Time series analysis, theoretical work and modelling efforts to quantify meteorologi-cal and solar effects on the middle atmosphere and thermosphere/ionosphere should be combined to provide more insight into forcing mechanisms of middle /upper atmosphere variability.

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Convener: Christoph Jacobi, jacobi@uni-leipzig.deInstitut für Meteorologie, Stephanstr. 3, 04103 Leipzig, GermanyPhone: +49-341-9732876

Co-Conveners: Katja Matthes, katja.matthes@gfz-potsdam.deHelmholtz-Zentrum Potsdam, Deutsches GeoForschungsZentrum GFZ, Telegrafenberg, A20 315, 14473 Potsdam, GermanyPhone: +49 331 288 1582, Fax +49 331 288 1163

Nicholas Pedatella, Nicholas.pedatella@colorado.eduNational Center for Atmospheric Research, High Altitude Observatory, 3080 Center Green Drive, Boulder, Colorado 80301, USA.Phone: +1 303 497 1514, Fax +1 303 497 1589

2.5 Middle atmosphere science

Papers related to any aspect of the dynamics, chemistry, or physics of the atmos-phere from near the tropopause to the lower thermosphere are appropriate for this ses-sion. Observational, modeling and theoretical papers are all solicited. Research topics include (but are not limited to): multiple-scale dynamics and mixing, observations and modeling of gravity waves, stratospheric chemistry and ozone, microphysics, chemistry and dynamics of the UTLS, and intraseasonal and interannual variations in the middle at-mosphere. In particular, investigations of the middle atmosphere in the context of climate of the whole atmosphere are encouraged.

Convener: Dan R. Marsh, marsh@ucar.eduAtmospheric Chemistry Division, National Center for Atmospheric ResearchP.O. Box 3000, Boulder, Colorado 80307-3000Phone: +1 303 497-1160, Fax: +1 303 497-1400

Co-Conveners: Andrew Charlton-Perez, a.j.charlton@reading.ac.ukDepartment of Meteorology, University of Reading, Earley Gate, PO Box 243, Reading, RG6 6BB, UKPhone: +44 (0) 118 378 6023

O. Morgenstern, o.morgenstern@niwa.co.nz NIWA Lauder, State Highway 85, Central Otago, Private Bag 50061, Omakau, New Zealand, Phone: +64 3 440 0421, Fax: +64 3 447 3348

Division 3 3.1 ULF waves space-ground coordination

ULF waves are a persistent feature of magnetised planets and are detected by

spacecraft and ground instrumentation over all magnetic activity levels. Observations and modeling of these waves provide information on changes of magnetospheric con-figuration , location of boundary regions, and the associated energy and mass transport processes. This symposium focuses on the detection and interpretation of ULF wave signals ranging from the irregular Pi activity to more continuous Pc1-5 waves and as-sociated space and space-ground relationships. These include, but are not limited to, waves in the vicinity of the magnetopause, polar cap ULF wave signatures, solar wind to magnetosphere wave transfer studies, global Pc waves in the outer magnetosphere, and ionospheric influences on ground ULF wave signatures. Due to the limited number

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of high-altitude spacecraft, ground-based observations are required to maximize the spatial-temporal coverage of magnetospheric dynamics that can be monitored by ULF waves. Contributions addressing the calibration of ground against spacecraft data are particularly welcome, in addition to comparisons that reveal propagation properties (or not) of these waves. Experimental and modeling studies of ULF waves in other planetary systems are also welcome.

Convener: Colin Waters, Colin.Waters@newcastle.edu.au

School of Mathematical and Physical Sciences, The University of Newcastle, Callaghan, 2308, New South Wales, AustraliaPhone: +61 2 4921 5421 Fax: +61 2 4921 6907

Co-Convener: Mark Engebretson, engebret@augsburg.edu Augsburg College, 2211 Riverside Avenue South, Minneapolis, MN 55454, USA., Phone: 612-330-1067, Fax: (612) 330-1649

3.2 ULF waves in the inner magnetosphere

Observations with multi-spacecraft missions as well as magnetometer arrays and radars with a large field of view continue to improve our understanding of the spatial and temporal structure of ULF waves in the magnetosphere. In addition, numerical tech-niques have advanced such that 3D MHD simulation is now capable of producing field line resonance and gyrokinetic code is being used to study ULF wave-particle interaction in the dipole magnetic field. This session invites papers on recent observational and theo-retical results on ULF waves in the inner magnetosphere, loosely defined to be the re-gion inward of geostationary orbit. Possible topics include, but not limited to, ULF waves generated by solar wind disturbances or internal plasma instabilities, plasmapause and ionospheric effects on wave propagation, and new observational, theoretical, or numeri-cal techniques. Papers specifically addressing the relationship between waves in space and on the ground should be submitted to Session 3.1. Papers specifically addressing wave-particle interaction in the radiation belt and ring current during geomagnetic storms should be submitted to Session 3.3.

Conveners: Kazue Takahashi, kazue.takahashi@jhuapl.eduSpace Physics Group (SRP), The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723-6099, USA, Phone: 240-228-5782, Phone: 240-228-0386

Co-Convener: Peter Chi, pchi@igpp.ucla.eduInstitute of Geophysics and Planetary Physics, University of California, 595 Charles Young Drive East, Los Angeles, CA 90095-1567, USA.Phone: +1-310-825-2040

3.3 Wave and particle dynamics in the radiation belts and ring current

Recent progress in the understanding of radiation-belt energization and loss pro-cesses, as well as ring-current build-up and decay, has shown that the system is highly variable, and relies on a variety of different waves and other transient phenomena to couple the dynamic processes occurring in the inner magnetosphere. Multiple energiza-tion and loss process occur simultaneously, over a variety of spatial scales ranging from microscopic wave-particle interactions, to global-scale interactions, and a variety of tem-poral scales, from milliseconds to hours. In this session, we will focus on the dynamical behaviour of radiation-belt and ring-current particles, the global variability and coupling to

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the inner magnetosphere, and the nature and spatiotemporal distribution of the underly-ing waves that control this behaviour.

Conveners: Jacob Bortnik, jbortnik@gmail.comDept of Atmospheric and Oceanic Sciences, Room 7115, Math Sciences Bldg., UC Los Angeles, CA 90095-1565, USA.

Co-Convener: Scot R. Elkington, scot.elkington@lasp.colorado.eduLaboratory for Atmospheric and Space Physics, University of Colorado, 1234 Innovation Drive, Boulder, Colorado 80303, USA.

3.4 Magnetospheric Boundary Layers

Physical processes and properties of the magnetospheric boundary layers are cru-cial in determining the solar wind impact on Earth’s magnetosphere. The main physical mechanisms that facilitate energy, momentum and plasma transport at the magneto-pause include Magnetic reconnection, Kelvin-Helmholtz Instability and diffusive mech-anisms such as wave particle-interactions. Recent multi-spacecraft missions such as THEMIS and Cluster have made it possible to observe these processes with multi-point measurements enabling calculations of gradients and distinction between temporal and spatial changes.

In this session we focus on the recent advances in boundary layer physics and properties. We welcome contributions from modelers, theorists and data-analysts to address the importance of boundary layer (magnetosheath, magnetopause, the cusps, high- and low-latitude boundary layer) processes and properties on magnetospheric dynamics.

Convener: Katariina Nykyri, nykyrik@erau.eduEmbry-Riddle Aeronautical University, 600 South Clyde Morris Blvd., Daytona Beach, FL 32114, USAPhone: 386-226-6714

3.5 Different response modes of the magnetosphere to solar wind driving

It is well known that magnetospheric activity is directly linked to the input of energy from the solar wind. In response to increased energy input associated with a southward component of the interplanetary magnetic field, the magnetosphere may store and re-lease this energy through a variety of response modes. These include, but are not lim-ited to, substorms, pseudo-breakups, steady magnetospheric convection, and sawtooth events. The coupling response is further complicated by seasonal effects and mass-loading of the magnetosphere by ion outflow. The unprecedented magnetospheric in situ measurements combined with extensive ground-based instrumentation and advanced simulations have greatly increased our knowledge of how the magnetosphere responds to different solar wind driving conditions. We invite investigations that examine the dif-ferent response modes of the magnetosphere, and how these responses manifest in all areas of geospace.

Convener: Larry Kepko, larry.kepko@nasa.govSpace Weather Laboratory, Code 674, NASA/Goddard Space Flight Center,Greenbelt, MD 20771, USAPhone: 301-286-2728, Fax: 301-286-9203

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3.6 The plasma sheet-ionosphere coupled system: Sinks, sources, transport and the roles of field-aligned currents and ion outflow

The plasma sheet serves as a reservoir for the storage of energy and mass that is central to magnetospheric dynamics. The plasma sheet is formed from particles entering directly and indirectly from the solar wind and ionosphere. The structure and asymmetry of its pressure, temperature, density, and entropy result from particle entry, transport, and loss processes that determine the dynamical magnetospheric response for differ-ent modes of solar wind driving. Plasma sheet dynamics are strongly coupled to the ionosphere through field-aligned currents and ion outflows. The ionosphere is modified by particle precipitation and Joule heating associated with field-aligned currents, while ionospheric outflows affect plasma sheet transport through mass loading. Furthermore, the Region 2 currents cause strong modifications of the global ionospheric electric field distribution, at middle latitudes by shielding and penetrating electric fields, at higher lati-tudes supporting the SAPS, and in the auroral region causing the Harang electric field reversal. Papers are solicited for this session on any of the above or related topics that are of importance to determining the formation of the plasma sheet (sources and losses), its structure and dynamics and/or the effects electrodynamical coupling has on iono-spheric and magnetospheric processes. Papers dealing with the system as a whole or the coupling processes are also appropriate.Convener: Jay Johnson, jrj@pppl.gov

Princeton University, Plasma Physics Laboratory, POB 451, MS 28, Princeton, NJ 08543-0000, USAPhone: +1 (609) 243-2603, Fax: +1 (609)243-2662

Co-Conveners: Elizaveta Antonova, antonova@orearm.msk.ruMoscow State University, Scobeltsyn Inst Nuclear Physics, Vorobievi Gori Moscow, 119991, RUSSIAPhone: 7-095-9412387, Fax: 7-095-939-0126

Larry Lyons, larry@atmos.ucla.eduDepartment of Atmospheric and Oceanic Sciences, UCLA405 Hilgard Ave., Los Angeles, CA 90095-1565, USAPhone: +1 (310) 206-7876, Fax: +1 (310) 206-5219

Hermann Luehr, hluehr@gfz-potsdam.deHelmholtz Centre Postdam, GeoForschungsZentrum (GFZ)Section 2.3 Telegrafenberg Potsdam, D-14473, Germany.Phone: 49-331-288-1735, Fax: 49-331-288-1235

Simon Wing, simon.wing@jhuapl.eduThe Johns Hopkins University, Applied Physics Laboratory, Laurel, Maryland 20723-6099, USAPhone: +1 (240) 228-8075, Fax: +1 (240) 228-1641

Sorin G. Zaharia, szaharia@lanl.govLos Alamos National Laboratory, POB 1663 MS D466, Los Alamos, NM 87545-0000, USAPhone: +1 (505) 667-0303, Fax: +1 (505) 665-7395

3.7 Auroral Processes

The auroral ionosphere and the field lines that thread it define a region of greatly en-hanced energy transfer between the solar wind, magnetosphere, ionosphere, and ther-mosphere. Decades of in-situ measurements and centuries of ground-based observa-tions have led to identification of key aspects of auroral physics, including the connection between auroral arcs and field-aligned currents, electric potential drops parallel to the

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geomagnetic field, and the role of ionospheric conductivity in determining the frequency and intensity of auroral arcs. However, there remains no widely-accepted, self-consistent theory able to account for the generation, morphology, particle acceleration and energy flux characterizing even the most common auroral forms. This session will provide a forum for new theoretical, experimental, and simulation results pertaining to all auroral phenomena. Critical reviews of the current state of understanding of the discipline are also encouraged.

Convener: David J. Knudsen, knudsen@ucalgary.caDepartment of Physics and Astronomy, University of Calgary2500 University Drive N.W., Calgary, AlbertaT2N 1N4 CANADAPhone 403-220-8651

3.8 High latitude electrodynamics and ion outflow

Ion outflow from the high-latitude ionosphere is continually flowing to the magneto-sphere, transferring particle energy and mass between the two regions. At times, the ionospheric outflow is the dominant source of magnetospheric plasma and therefore plays a critical role in the dynamics of magnetospheric substorms and geospace magnet-ic storms. Conversely, high-latitude electrodynamics is influenced by the interplanetary magnetic field (IMF), the magnetospheric convection electric field and by currents and impulsive electric fields associated with substorms. Understanding the complex coupling of high-latitude electrodynamics, ionospheric outflow and magnetospheric dynamics, is of vital importance to space physics. Papers on modeling studies and ground- and space-based multi-instrument observations of this coupling are solicited. Comparisons of numerical simulations with observations from multiple platforms are particularly suitable to this session.

Convener: Ioannis A. Daglis, daglis@space.noa.grInstitute for Space Applications and Remote Sensing, National Observatory of Athens, Metaxa and Vas. Pavlou St., Penteli, 15236 Athens, GreecePhone : +30-210-8109185, 8109182, Fax: +30-210-6138343

3.9 Reporter Reviews - Division III

New and interesting research from Division III scientists published in 2011-2013 will be summarised by the Reporters, following eight themes: (1) Magnetopause and boundary layer, (2) Auroral phenomena, (3) ULF waves, (4) Tail dynamics, (5) Inner-magnetosphere, (6) Wave-particle interaction in the inner-magnetosphere, (7) Global magnetospheric dynamics, and (8) Magnetospheres other than Earth.

Convener: Clare Watt, watt@ualberta.caDepartment of Physics, University of Alberta, Edmonton, Alberta, Canada T6G 2G7Fax: +1 780 492 7014

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Division 4 4.1 New Solar and Interplanetary Results

This session is dedicated to the new observational results from recent missions (such as SDO, Hinode, Stereo, SOHO, Cluster) about the dynamics and structure of the Sun and the interplanetary medium, and relevant theoretical and modelling work. These results have enriched our knowledge of the energy storage and release processes of solar eruptions including flares and CMEs, the heating of the corona, the origin and acceleration of the solar wind, the acceleration and transport of energetic particles, MHD shocks, wave-particle interactions, and plasma turbulence, etc. This session invites contributions that emphasize new results from both space and ground-based observatories, as well as the development of theories and models which are relevant to our understanding the dynamics of the sun and interplanetary medium. It is aimed at stimulating exchanges and promoting discussions on the results derived from the new observations and latest research in the field.

Convener: Yao Chen, yaochen@ustc.edu.cnCenter for Space Weather (CSW), Shandong University at WeihaiWeihai Shandong, China 264209Phone: +86-631-5673638

Co-conveners: Huw Morgan, hum2@aber.ac.uk Institute of Mathematics and Physics, Aberystwyth University, Aberystwyth, Ceredigion, SY23 3BZ, UK Tel: 01970 622 802 Fax: 01970 622 826

Ying Liu, liuxying@ssl.berkeley.eduSpace Sciences Laboratory, UC Berkeley, 7 Gauss Way, Berkeley, CA 94720, USA. Phone: (510)642-8040

4.2 Wave Propagation in the Outer Solar Atmosphere

In recent years wave heating and acceleration mechanism have come to the fore in solar physics following a dramatic increase in observational capabilities. This session will discuss wave and quasi-periodic phenomena as they are observed throughout the outer solar atmosphere. We would like to explore the large variety of drivers and cou-pling mechanisms for these phenomena as well as making a careful assessment of their energy content and dissipation mechanisms in open and closed magnetic topologies.

Convener: Scott W. McIntosh, mscott@ucar.eduNational Center for Atmospheric Research (Room 3624) High Altitude Observatory, 3080 Center Green Drive - CG1, Boulder, CO 80301, USA.Phone: 303 497 1544, Fax: 303 497 1589

4.3 Multi-spectral studies of solar flares

Solar flares are often viewed as the most dramatic and powerful magnetic explosions in the solar system. After the deep solar minimum of 2008-2009, the solar activity is on

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the rise and the Sun has already produced a number of spectacular solar flare events. Despite of the substantial progress made over the last few decades in understanding the physics of solar flares, there are many open questions. Over the last few years, the unprecedented variety of the spacecraft and ground based observations of solar flares become available: from the high energy gamma and X-ray emission (RHESSI, Fermi), through EUV, optical (SDO, Hinode, STEREO) range down to radio frequencies (STEREO, Wind). These space-based observations are substantially enhanced via a number of ground based observations, notably with solar radio observatories. The ses-sion aims to bring together the diverse solar flare community to discuss the latest obser-vations, modelling and theoretical developments in the area of solar flare physics. It will focus on correlative analysis of simultaneous multi-spectral observations of solar flare phenomena addressing the key science questions of magnetic energy release, energetic particle acceleration and transport, the response and emissions in the solar atmosphere and the heliosphere. In addition, the connection of the observational results with the modelling and theoretical developments in this area will be discussed.

Convener: Eduard Kontar, Eduard.Kontar@glasgow.ac.ukSchool of Physics and Astronomy, University of Glasgow, Glasgow G12 8QQ , U.K.Phone: +44 141 330 2499, Fax: +44 141 330 8600

Co-Conveners: Nicole Vilmer, nicole.vilmer@obspm.frLESIA, Observatory of Paris, FrancePhone: +33-1-4507-7806, Fax +33-1+4507-7959

Sam Krucker Space Sciences Laboratory, UC Berkeley, 7 Gauss Way, Berkeley, CA 94720, USAPhone: (510) 643-310, Fax: (510) 643-8302

Gregory Fleishman, gfleishm@njit.eduDepartment of Physics, New Jersey Institute of Technology, University Heights, Newark, New Jersey 07102-1982, USAPhone: (973) 596-5569

4.4 Crossing the Heliopause into the Interstellar Medium

Recent Voyager 1 data shows the radial speed of the plasma in the heliosheath is near zero. This signature suggests that Voyager 1 may be near the heliopause and about to cross into the interstellar medium. Recent data from IBEX suggests that no bow shock is formed in the interstellar medium so Voyager will sample unshocked interstellar mate-rial. This session will cover recent observations by both Voyager and IBEX and model results bearing on the interaction of the heliosphere with the interstellar medium and in particular the heliopause interface.

Convener: John Richardson, jdr@space.mit.edu Kavli Center for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA;Phone: 617/253-6112, Fax: 617/253-0861

Co-Convener: Iver Cairns, cairns@physics.usyd.edu.auSchool of Physics , University of Sydney, Sydney, NSW 2006, AustraliaPhone: +61-2-9351-3961, Fax: +61-2-9351-7726

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4.5 Reporter Reviews

In this session, in-depth review talks will report major recent observational and theo-retical progresses on the sun, the solar wind and heliosphere. Given by experienced and active researchers, these talks cover a comprehensive range of topics and debates which are relevant to Division IV scientists and appealing to researchers in other IAGA divisions. All talks in this session are by invitation only.

Conveners : Xing Li, xxl@aber.ac.ukInstitute of Mathematics and Physics, Aberystwyth University Penglais road, Aberystwyth SY23 3BZ, United KingdomPhone: +44 1970 621542, Fax: +44 1970 622826

John Richardson, jdr@space.mit.eduMIT 37-655, Massachusetts Institute of Technology, Cambridge, MA 02139, USA.Phone: +1 617-253-6112, Fax: +1 617 253-0861

Division 5 5.1 Advances towards an improved global geomagnetic observatory network

Geomagnetic observatories provide magnetic vector time series that are of special value because of their homogenous, continuous, and long period absolute data. This session deals with advancements in the operation of individual observatories as well as the progress of the global geomagnetic observatory network. The global coverage can be improved by establish-ing new observatories, and such effort is currently ongoing. The time series of the existing observatories have to be continued and might even be prolonged backwards by digitizing in-formation from analogue magnetograms and tables. Geomagnetic observatory data has to be accessible to scientists in a fast and uniform way. Contribution are invited on the mentioned subjects, including geomagnetic observatory instrumentation and operation, processing and data management, digitization of analogue data, quality check of archive data, new data prod-ucts like Intermagnet’s quasi-definitive and 1-second data, and on remote observatories.

Convener: Jürgen Matzka, jrgm@space.dtu.dkDTU Space, Elektrovej, bygn. 327DK - 2800 Kgs. Lyngby, DenmarkPhone: +45 3532 5700, Fax: +45 353 62475

Co-Conveners:Pavel Hejda, ph@ig.cas.czInstitute of Geophysics AS CR, Bocni II/1401, 141 31 Prague, Czech RepublicPhone: +420 267103339, Fax: +420 272761549

Katia Pinheiro, kpinheiro@on.brObservatório Nacional/MCT, Rua General José Cristino, 77 - São Cristóvão, Rio de Janeiro, RJ - Brasil CEP: 20921-400Phone: +55 (21) 3504-9286, Fax: +55 (21) 2580-7081

5.2 Recent magnetic surveys for regional and global characterization of the geomagnetic field

Over the past decades, geophysical surveys of the Earth’s magnetic field have been significantly advanced through the use of satellite technology permitting global field characterization. Large-scale airborne, land and marine geomagnetic surveys remain

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an important source for detailed regional near surface data. The combination of remote sensing and ground survey measurements through generation of seamless digital grids has resulted in new data sets describing crustal magnetic anomalies across many re-gions of the globe.

This session focuses on applications and case studies of geomagnetic surveys provid-ing surface (land and marine) and airborne magnetic data, as well as the interpretation of this data with respect to the spatial and temporal evolution of the Earth’s magnetic field. Additionally, we invite papers on magnetic studies for the understanding of regional tecton-ics, natural hazards and environmental settings, as well as contributions concerning the development of related data acquisition methodology, technology and its interpretation.

Convener: Barbara Leichterbarbara.leichter@zamg.ac.atDepartment Geomagnetism and Gravity, Bereich DMM / Division DMMZAMG - Zentralanstalt für Meteorologie und Geodynamik, 1190 Wien, Hohe Warte 38Phone: +43 1 36026 2515, Fax: +43 1 368 66 21

Co-Conveners: Aude Chambodut, aude.chambodut@unistra.frDepartment of Geomagnetic Observatories, EOST, 5 rue Rene Descartes, 67084 Strasbourg Cedex, FrancePhone: +33 (0)3 68 85 00 81, Fax: +33 (0)3 68 85 01 25

Kusumita Arora, kusumita@ngri.res.inMagnetic Observatory, CSIR-NGRI, Hyderabad 500007Phone (off): +91 40 23434773, mobile +919866234680

5.3 Magnetic observatory data as applied in space weather/climate

Ground magnetometers can be used to study the magnetic fields and electric currents of the changing space environment. Magnetic observatories and networks have provid-ed and continue providing important long-term data sets for monitoring space conditions over many solar cycles. This valuable global database allows us to explore both short-term changes of space weather and the long-term evolution called the space climate. In this session we solicit papers that address any of a versatile range of topics related to geomag-netic observations and geomagnetic indices such as: special space events and process-es; derivation and properties of indices of geomagnetic activity and magnetic storminess; short-term and long-term drivers of magnetic disturbances and storms and their relation to the Sun; geomagnetic observations and indices in research and applications; geomagnetic data mining, analysis, validation, assimilation and visualisation; short-term variability of the space environment and space weather; and long-term variability and space climate; mod-els of magnetospheric and ionospheric current systems and fields.

Convener: E. Joshua Rigler, erigler@usgs.govUSGS Golden, Box 25046, MS966, DFC, Denver CO 80225, USA Phone: 303-273-8607, Fax: 303-273-8600

Co-Convener: Kalevi Mursula, Kalevi.Mursula@oulu.fiDepartment of Physical Sciences, P.O. Box 3000, FIN-90014 University of Oulu, Finland. Phone: +358-8-5531366, Fax +358-8-5531287

5.4 Polar cap geomagnetic indices: meaning derivation and uses

The Polar cap (PC) index is a set of geomagnetic indices (PCN and PCS) which were originally designed to be a proxy for the electric field in the solar wind determined using

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IAGA Meeting 2013

geomagnetic measurements from ground stations under the polar cap. The indices have been in use now for 25 years (concept suggested in 1988) therefore it is a rather new topic in the field of geomagnetic indices, as compared to the planetary indices that inherit the knowledge accumulated since the late 19th century, or to ring current characteriza-tion that began in the nineteen-fifties!

Much literature has been published during the last fifteen years, with nomenclatures and methods that evolve with time so as to improve the index and get the most reliable possible information on the convection in the polar ionosphere.

Since 1997 discussions of the validity of the index to be endorsed as an official IAGA index have ensued. There is no doubt as to the scientific merit of the index. Clarification of the PC index issues would be of great help to pave the way towards a definition of the PC index that gains consensus within the scientific community. This session aims at contributing to this clarification. Contributions dealing with the determination, meaning, and usage of Polar Cap geomagnetic indices are welcome

Convener: Michel Menvielle, michel.menvielle@latmos.ipsl.frISGI/LATMOS 4, Avenue de Neptune, F-94107 Saint Maur Des Fosses, France, Phone: 0144279234

Co-Conveners: Heather McCreadie, bilbysan@gmail.comSchool of Physics, Durban, University of KwaZulu-Natal, Westville Campus, University Road, Westville, Private Bag X5400, Durban 4000, South Africa, Phone: +27 31 260-7662, Fax: +27 31 260 7795)

Crisan Demetrescu, crisan@geodin.roInstitute of Geodynamics of the Romanian Academy, 19-21 Jean-Luis Calderon St., RO-020032, Bucharest-37, Romania.Phone: (4021)317.21.26, Fax:(4021)317.21.20

5.5 The use of Geomagnetic observations in conjunction with lidar, radar and oth-er measurements for ionospheric studies

An important aspect of ionospheric studies is the coupling provided by forcing be-low apart from the forcing from above induced by space weather events. The quiet-time variabilities of ionosphere are primarily caused by atmospheric waves and tides that can explain the day-to-day variability of several ionospheric parameters. In recent years, sat-ellite observations have focused on understanding the wave-4 signatures noticed in a variety of data sets, including geomagnetic field observations. When combined with other complementary observations from lidars and radars, greater use of ground and satellite magnetic field data in addressing the day-to-day variability of the ionosphere is envis-aged. There has also been considerable interest in the recent past in understanding the ionospheric signatures of earthquakes, volcanic eruptions, thunderstorms and cyclones/typhoons though the mechanisms by which the disturbances propagate to ionosphere are still being debated. This session will focus on all aspects of atmosphere-ionosphere, lithosphere-ionosphere and magnetosphere-ionosphere-atmosphere coupling with em-phasis on the role of geomagnetic, lidar, radar and barometric observations from ground and a variety of satellite data sets in addressing those aspects.

Convener: Subramanian Gurubaran, gurubara@iigs.iigm.res.inEquatorial Geophysical Research Laboratory, Indian Institute of Geomagnetism, Krishnapuram, Tirunelveli 627 011, India Phone: 0091-462-2521465, Fax: 0091-462-2521466

Co-Conveners: Jennifer L. Gannon, jgannon@usgs.govUSGS Geomagnetism Program, USGS DFC, Box 25046, MS 966,

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Denver, CO 80225-0046, USAPhone: +1-303-273-8487, Fax: +1-303-273-8506

Akimasa Ieda, ieda@stelab.nagoya-u.ac.jpSolar-Terrestrial Environment Laboratory, NagoyaUniversity, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, JAPANPhone: +81-52-747-6336, Fax:+81-52-747-6334

5.6 Modelling and interpretation of lithospheric magnetic anomalies

We invite contributions on lithospheric and crustal magnetic anomalies at all scales, from the analysis of a wide range of datasets including magnetic satellite missions, aero-magnetic and marine magnetic surveys, and ground magnetic measurements (including archaeological investigations). Contributions involving different scales and/or datasets are particularly welcome, including results derived from data compilations such as the World Digital Magnetic Anomaly Map. Contributions on methodological advances to ac-quire, process, interpret and model magnetic anomalies are also expected. Finally, origi-nal contributions on seafloor spreading magnetic anomalies are encouraged to celebrate the 50th anniversary of Vine and Matthews (1963) seminal paper on their modelling and interpretation.

Convener: Jérôme Dyment, jdy@ipgp.frLaboratoire de Geosciences Marines, Institut de Physique du Globe de Paris, CNRS UMR 7154, 1 rue Jussieu, 75005 Paris, FrancePhone: (33) (0) 1 83 95 76 56, Fax (33) (0) 1 83 95 77 10

Co-Conveners: Dhananjay Ravat, dhananjay.ravat@uky.eduEarth & Environmental Sciences, University of Kentucky 101 Slone Building, Lexington KY 40506-0053, USAPhone: (859) 257-3758, Fax. (859) 323-1938

Juha V. Korhonen, juha.korhonen@gtk.fi Espoo Unit, Geological Survey of Finland, P.O. Box 96. 02151 Espoo, Finland Phone: 358 205502275

5.7 Reporter Reviews

Scope: This session is composed of invited papers which review recent progress, innovation or discovery in observation, modelling and interpretation of the geomagnetic field. All Division-V research topics are covered: geomagnetic data acquisition systems; magnetic field observations (ground and satellite measurements and survey programs); field modelling and interpretation; geomagnetic indices; data dissemination and analysis; all to improve understanding of the geomagnetic field and its various sources, from core to space.

Conveners: Alan W P Thomson, awpt@bgs.ac.ukBritish Geological Survey, West Mains Road, Edinburgh EH9 3LA, UKPhone:+44 (0) 131-650-0257 (direct), +44 (0) 131-667-1000 (switchboard)

Co-convener: Pieter Kotze (SANSA, South Africa), pkotze@sansa.org.zaHermanus Magnetic Observatory, P O Box 32, Hermanus 7200, South AfricaPhone: +227 283 21196

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ICDC and IDCH

Sessions of ICDC and IDCH all are organized together with other IAGA divisions, please check above!

Mexico

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Programme Committee

ChairIAGA Secretary General: Mioara Mandea Centre National D’Etudes Spatiales,

2, Place Maurice Quentin, 75001 Paris, France; E-mail: iaga_sg@gfz-potsdam.de, Phone: +33 1 44 76 79 48

MembersDivision I Chair: Gauthier Hulot (France) gh@ipgp.fr

Division II Chair: Dora Pancheva (Bulgaria) dpancheva@geophys.bas.bg

Division III Chair: Larry Kepko (USA) larry.kepko@nasa.gov

Division IV Chair: Xing Li (UK) xxl@aber.ac.uk

Division V Chair: Alan Thomson (UK) awpt@bgs.ac.uk

Chair of Interdivisional Commission on History: Ronald Doel (USA) rdoel@fsu.eduChair of Interdivisional Commission on Developing Countries: Inez S. Batista (Brazil) inez@dae.inpe.brChair of Interdivisional Working Group on Education and Outreach: Eduard Petrovsky edp@ig.cas.cz

National Advisory Committee Jose Valdés President of National Body of IUGG

Carlos Aramburo Vice-President, Universidad Nacional Autónoma de México

Avtandil Gogichaishvili President of the Unión Geofísica Mexicana

José Franco President of the Academia Mexicana de Ciencias

Leticia Torres Co-Chair Consejo Nacional de Ciencia y Tecnología

Gerardo Carrasco Director of the Centro de Geociencias, UNAM

Francisco Graef Director of the Centro de Investigación Científica y de Educación Superior de Ensenada Baja California

Mexico

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IAGA Meeting 2013

Scientific Freedom Policy StatementThe organisers of the IAGA 2013 Scientific Assembly shall observe the universality

of science and shall affirm the rights of scientists throughout the world to adhere to or associate with international scientific activity without discrimination based on citizenship, religion, creed, political stance, ethnic origin, race, colour, language, age or sex, in ac-cordance with the statutes of the International Council of Scientific Unions (ICSU).

Liability and InsuranceThe organisers cannot accept liability for any personal accidents, loss of belongings

or damage to private property of participants and accompanying persons that may occur during the Congress. Participants are advised to make their own arrangements to obtain health, travel and property insurance before their departure.

Travel to MéridaPassport and Visa

For exact information please contact the Mexican Embassy or Consulate in your country and/or the local Authorities. In case of problems please contact the local LOC.

For entry to Mexico you need to show the following documents:• Valid passport or equivalent travel documents acknowledged by the Mexican

authorities,• Valid visa, where necessary, for entry or transit,• Papers proving the purpose of the voyage and stating means of transportation,

accommodation and local expenses, may be useful.

By PlaneMérida International Airport is situated about 10 km from Mérida City centre. Transport

to the city is organized by authorized taxis and shared shuttle services at fixed prices, to be hired in the airport. Do not hire unauthorized taxis outside the airport, or offered by individuals within the airport.

Cancun International Airport is located about 300 km from Mérida. Arriving in Cancun you can travel by first class bus to Mérida, directly from the airport to the hotel Fiesta American, one of the meeting venues (travel time ~4 hours, see:http://www.ado.com.mx/wadod/compra.jsp or http://www.ticketbus.com.mx/wtbkd/I18n.tb?language=en&region=US).

By CarTaking a rental car at Cancun Airport is also easy and you can take the toll highway

to Mérida.

Payment is in Mexican Pesos or by credit cardsee currency exchange rates in:http://www.banamex.com/economia_finanzas/en/divisas_metales/resumen.htm

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Hotel ListWe blocked a limited number of hotel rooms at special prices. All indicated prices are

per person and night and do not include any taxes (mainly 16% VAT), and breakfast only where stated. When paying with an international credit card, ask at the hotel front desk for the VAT exemption (“taza zero”, which is only applicable for hotel accommodation without food).

Reservation has to be made directly with the hotels using their email address and reservation code (see below), before June 1, 2013. You will need to use a credit card for guarantee. Cancellation is only possible before June 30, 2013. More details about the hotels are listed on their websites indicated below. In case you can not use a credit card, please contact the LOC to arrange for a one night deposit on the conference account.

If you need help in finding a room mate, please also contact the LOC by e-mail, loc@iaga2013.org.mx

Fiesta Americana Mérida Hotel ***** (Congress venue) 1Deluxe room single person US$ 109.00

Deluxe room two persons US$ 54.50 -Main Hotel-Reservation code: “Congreso IAGA 2013”htttp://www.fiestamericana.com.mx; rinternet@posadas.comToll free 01 800 504 5000, from USA and Canada (1 800) FIESTA 1

Hotel Presidente Intercontinental ***** 2Deluxe room single person US$ 109.0

Deluxe room two persons US$ 54.50 80 m from Main HotelReservation code: “IA8”http://www.ichotelsgroup.com/intercontinental/hotels/gb/en/merida/midha/hoteldetail; susana_coba@grupopresidente.comPhone: (52) 01 9999 42 9000

Holiday Inn Hotel Mérida ***** 3Deluxe room single person US$ 95.00

Deluxe room two persons US$ 47.50 70 m from Main HotelReservation code: “IAG”http://www.holidayinn.com/hotels/us/en/reservation; reservaciones2@hinnmerida.com – ibass@hinnmerida.comPhone: (52) 01 9999 42 88 00 – (52) 01 9999 42 88 11,with Carlos Rodríguez

El Español Hotel (Paseo de Montejo) 4Deluxe room single person US$ 85.50

Deluxe room two persons US$ 49.00 300 m from Main HotelReservation code: “IAGA2013”http://www.elespanoldemontejo.com/index_i.htm, ventas2@elespanoldemontejo.com – ventas@elespanoldemontejo.com

Phone: (999) 9230880

El Español *** 5Deluxe room one person US$ 50.00

Deluxe room two persons US$ 29.00 1.5 km from Main Hotel

Deluxe room three persons US$ 21.00

Deluxe room four persons US$ 16.00Reservation code: “IAGA 2013”http://www.hotelelespanol.com.mx/home.php?idioma=eng, reservaciones@hotelespanol.com.mxPhones: (52) 01 9999 23 28 54 – (52) 01 9999241036 with Fátima Beatriz Montalvo Ibarrra

[ U ; f B W Y c 8 WiFi � u

[ U T L ; f B W Y c 8 WiFi �

[ U T L ; f B W Y c 8 WiFi �

U ; f B 8 WiFi

[ U ; f B W 8 WiFi �

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[ Special need facilities

U Safety-deposit boxes

T Laundry and dry-cleaning

L Foreign currency exchange

; Parking

Hotel Misión Panamericana **** 6Standard room one person US$ 60.50

Standard room two persons US$ 30.50 950 m from Main HotelReservation code: “IAGA”http://www.hotelesmision.com/Home.aspx?Preserve=1;ejecutivomerida3@hotelesmision.com.mx; reservacionesmerida@hotelesmision.com.mx with: Lic. Arely Peña

Phone: (999) 9 23 94 07 ext. 228, call center: 01 800 900 3800

Hotel Castellano **** 7Deluxe room one person $ 80.50

Deluxe room two persons $ 40.50 800 m from Main Hotel

Deluxe room three persons $ 30.50

Deluxe room four persons $ 26.00Reservation code: “Castellano IAGA”http://www.elcastellano.com/english/, reservations@elcastellano.com – alopez@elcastellano.comPhone: (52) 01 9999 300100 with Lic. Alejandra López

Hotel Caribe *** 8Standard room one person $52.50

Standard room two persons $27.00 850 m from Main Hotel

Standard room three persons $19.50

Standard room four persons $16.50Reservation code: IAGAhttp://www.hotelcaribe.com.mx/index.php, reservaciones@hotelcaribe.com.mxPhone (52) 01 9999 24 90 22, toll free: 01 800 712 0003, with Cuxtali

Hotel La Misión de Fray Diego **** 9Standard room one person $98.50

Standard room two persons $49.00 960 m from Main Hotel

Standard room three persons 36.50Reservation code: IAGAhttp://www.lamisiondefraydiego.com/index.php, res@lamisiondefraydiego.comPhone: (52) 01 9999 24 11 11, toll free: 01 800 221 0599

U T L ; B W 8 WiFi �

[ U ; f W B 8 WiFi �

f Transportation

B Restaurant

W Pool

Y Babysitter on request

c Medical services

8 Business centre

WiFi Internet access

� Fitness center

u Pet friendly

[ T ; f B W c WiFi �

T B W c WiFi �

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Mérida Cathedral

1. Fiesta Americana Mérida Hotel

2. Hotel Presidente Intercontinental

3. Holiday Inn Hotel Mérida

4. El Español Hotel (Paseo Montejo)

Castellano5. Hotel

6. El Español

7. Hotel Misión Panamericana

Hotel Caribe8.

Hotel La Misión de Fray Diego9.

6

7

5

8

1

4

9

2 3

Hotels map

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IAGA Meeting 2013

A few words about Mexico exicoMMexico is located in North America, embraced by the Gulf of Mexico to the

east and the Pacific Ocean to the west. Mexico’s northern neighbour country is the United States of America and its southern neighbours are Guatemala and Belize. Mexico’s geography is divided in North and South by a volcanic belt that runs from the Pacific Ocean to the Gulf of Mexico. Mexico’s northern region is dominated by desert climate, the World’s largest ignimbrites cover is located in the north-western region; the Baja California Peninsula forms part of the Pacific Plate, while the rest of Mexico forms part of the North America plate, which makes this region one of the most active tectonic provinces in the world the Gulf of California opens at a velocity of 6.0 cm/year. The Trans-Mexican Volcanic Belt, covers most of central Mexico and is characterized by the presence of both inactive and active volcanoes. Three of these volcanoes (Popocatepetl: “The smoking mountain”, Iztaccihuatl: “The white woman” and Citlaltepetl: “The Star’s mountain”) are the closest to the Equator with perma-nent glaciers. South of the volcanic belt, Mexico’s geography and geology is more complicated, ranging from rain forests in Chiapas to the jungles of Yucatan. The eastern coast of the Yucatán Peninsula runs along the Mexican Caribbean where one the World’s most important coral reefs is located with Cancun as the most important resort in Mexico.

Mexico’s history has been enriched by several prehispanic cultures like the Toltec, Zapotec, Mayan and many others in its origins. Later on, from the 11th to 16th century the Aztec Empire ruled over most of Mesoamerica until the encounter with the Spanish in the late 15th century and finally the Conquistadors took over the Empire in 1521. From then on, the New Spain became one of the most important assets of the Spanish Crown, some of the more important contributions from the New Spain to the world are: tobacco, tomato, turkey, maize, vanilla and chocolate. Present day Mexico is a vibrant nation that is working its way to modern times with a population of 120 million inhabitants with Mexico City, Guadalajara and Monterrey as the most important cities. The Universidad Nacional Autónoma de México (UNAM) has been ranked among the 50 most important universi-ties in the World.

The venue: YucatánYucatán is located within the Yucatán Peninsula in eastern Mexico. The

weather is usually hot and humid in the end of August. The average tempera-ture in August is 35 °C. The standard nominal voltage in Mexico is 110 V (60 Hz, AC). The official currency in Mexico is the Mexican Peso. US Dollars or Euros can be changed at banks and at exchange points located in the

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city.All major credit cards are accepted in Mexico in places displaying the emblem at the entrance. Mexico has an extensive network of ATM where you can get cash with Visa, MasterCard and other common bank cards.

History of MéridaThere were three Spanish conquistadors named "Francisco de Montejo":

Francisco de Montejo "el Adelantado" ("The Lieutenant", the eldest), Francisco de Montejo y León "el Mozo" ("The Boy", his son), and Francisco de Montejo "el Sobrino" ("The Nephew"). Mérida was founded in 1542 by Francisco de Montejo y León ("el Mozo") and named after the town of Mérida in Extremadura, Spain. It was built on the site of the Maya city of T'hó, which was also called Ichkanzihóo orIchcaanzihó; "City of Five Hills") in reference to its pyramids. T'ho had been a center of Mayan culture and activity for centuries: because of this, some historians consider Mérida the oldest con-tinually-occupied city in the Americas.

Carved Maya stones from ancient T'ho were widely used to build the Spanish colonial buildings that are plentiful in downtown Mérida, and are visible, for instance, in the walls of the main cathedral. Much of Mérida's architecture from the colonial period through the 18th century and 19th cen-tury is still standing in the "centro histórico" of the city. From colonial times through the mid 19th century, Mérida was a walled city intended to protect the Peninsular and Criollo residents from periodic revolts by the indigenous Maya. Several of the old Spanish city gates survive, but modern Mérida has expanded well beyond the old city walls.

Late in the 19th century and the early 20th Century, the area surrounding Mérida prospered from the production ofhenequén. For a brief period, around the turn of the 20th century, Mérida was said to house more millionaires than any other city in the world. The result of this concentration of wealth can still be seen today. Many large and elaborate homes still line the main avenue called Paseo de Montejo, though few are occupied today by individual fami-lies. Many of these homes have been restored and now serve as office build-ings for banks and insurance companies.

Mérida has one of the largest centro historico districts in the Americas (surpassed only by Mexico City and Havana, Cuba). Colonial homes line the city streets to this day, in various states of disrepair and renovation; the historical center of Mérida is currently undergoing a minor renaissance as more and more people are moving into the old buildings and reviving their former glory.

In June 2007, Mérida moved its city museum to the renovated Post Office building next to the downtown market. The Museum of the City of Mérida houses important artifacts from the city's history, as well as an art gallery.

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IAGA Meeting 2013

Local Organising CommitteeIAGA 2013 LOCBlvd. Juriquilla No. 3001, Querétaro, 76230, Mexico. Tel: +52 442 238 1004www.iaga2013.org.mx, loc@iaga2013.org.mx

Chair Harald Böhnel Phone: +52 442 238 1004, ext. 109, hboehnel@geociencias.unam.mx

Co-chair Román Pérez Phone: +52 442 238 1004, ext. 105, roman@geociencias.unam.mx

Co-chair Mérida Mario Rebolledo Phone: +52 999 942 8330, ext. 208, marior@cicy.mxSecretary Roberto Molina Phone: +52 442 238 1004, ext. 126, rmolina@geociencias.unam.mxTreasurer Jorge Arzate Phone: +52 442 238 1004, ext. 111, arzate@geociencias.unam.mxExcursions Luis Alva Phone: Phone: +52 55 562 24237, lalva@geofisica.unam.mxSponsors contact Blanca Mendoza

Tel +52 55 562 24 113, blanca@geofisica.unam.mxWeb master Victor de la Luz

Tel +52 222 266 3100, ext 1315, itztli@gmail.comTechnical editor J. Jesús Silva

Tel +52 442 238 1004, ext. 193, jsilvac@geociencias.unam.mxComputing and Emilio Navainternet services Phone: +52 442 238 1004, ext. 121, enava@geociencias.unam.mx

Juan Manuel López Phone: +52 442 238 1104, ext. 165, jmlopez@geociencias.unam.mx

Luna Maya DMC Angelica Luna& Meetings Phone: +52 999 935 6599, aluna@lunamayadmc.com.mxPlaner

Mexico

Further Members of the LOC:Ernesto Aguilar, Cecilia Caballero, Edgardo Cañón, Gerardo Cifuentes, Xochitl Blanco, Américo González, Esteban Hernández, Héctor López, Dolores Maravilla, Juan Julio Morales, Mario Rodríguez, José Romo, Vsevolod Yutsis.

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Joint sessions Div. I Div. II Div. III Div. IV Div. V ICDC IDCH

Monday 26

a.m. 1.1, 1.2, V 1.6 1.12 2.1 2.5 3.3 4.1 5.1 - -p.m. 1.6 1.12 2.1 2.5 3.3 3.2 4.1 5.1 - -posters 1.6 1.12 2.1 2.5 3.3 4.1 5.1 - -

Tuesday 27

a.m. II, III 1.1 1.5 1.8 2.1 2.5 3.2 4.1 5.2 - -p.m. 1.1 1.5 1.8 2.2 2.5 3.1 4.1 5.2 5.3 - -posters 1.1 1.5 1.8 2.2 3.1 3.2 5.2 - -

Wednesday 28

a.m. 1.2, II, IV,V, IDCH

1.3 1.10 2.3 3.1 3.6 4.2 5.3 -

p.m. 1.3 1.10 2.3 3.6 4.2 5.3 -

posters 1.3 1.10 2.3 3.6 4.2 5.3 -

Thursday 29

a.m. 1.2, II, IV 1.4 1.7 2.3 3.9 4.2 5.4 - -p.m. 1.4 1.7 3.8 3.9 4.3 5.6 - -posters 1.4 1.7 2.3 3.9 5.4 5.6 - -

Friday 30

a.m. 1.1, II 1.2 1.9 2.4 3.8 3.7 4.3 5.5p.m. 1.2 1.9 2.4 3.7 4.3 4.5 5.5posters 1.2 1.9 2.4 3.8 3.7 4.3 5.5

Saturday 31

a.m. II, ICMA, IDCH 1.11 1.13 3.4 3.5 4.4 5.7

p.m. 1.11 1.13

posters 1.11 1.13 3.4 3.5 4.4 5.7

Division´s Activities per Day

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Division´s Activities per Day

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www.iaga2013.org.mx