3d European Space Weather Week – November 13-17, 2006, Brussels, Belgium Ring current models: How well can they be applied for space weather modeling purposes?

3d European Space Weather Week – November 13-17, 2006, Brussels, Belgium

Ring current models: How well can they be applied

for space weather modeling purposes?

N. Yu. Ganushkina, T. I. Pulkkinen (Finnish Meteorological Institute, Space Research, Helsinki, Finland),

A. Milillo (Istituto di Fisica dello Spazio Interplanetario, Rome, Italy),

M. Liemohn (University of Michigan, Space Physics Research Laboratory, USA)

J. Geophys. Res., 111, A11S08, doi:10.1029/2006JA011609, 2006

Outline Following the evolution of proton ring current during the GEM IM/S Challenge storm event on April 21-25, 2001 using three ring current models: - the ring current model combined with tracing particles numerically in the drift approximation by Ganushkina et al., Ann. Geophys., 23, 579-591, 2005; - the empirical model of proton fluxes in the inner magnetosphere by Milillo et al., J. Geophys. Res., 108, doi:10.1029/2002JA009581, 2003; - the kinetic ring current-atmosphere interaction model (RAM) by Liemohn et al., J. Geophys. Res., 106, 10,883-10,904, 2001.

Focus on contributions from protons in different energy ranges to the ring current energy during different storm phases (base: Polar CAMMICE/MICS observations).

Study the influence on the model ring current energy of the - choice of magnetic and electric field models, - initial particle distributions, - role of substorm-associated electric fields in particle transport and energization.

Discussion on outputs from different models.


April 21-25, 2001: Storm event overview


Shock arrival: small Vx junp of 100 km/s, large density pulse with Psw to 10 nPa, IMF Bz > 0 at 2145 UT Apr 21, SYM-H from 0 to 30 nT, no AE increase, Kp around 3

Cloud arrival: IMF Bz < 0 at 0130 UT Apr 22, Vx from 400 km/s to 300 km/s, Psw fluctuating at 3 nPa, SYM-H negative reaching -100 nT at 1540 UT Apr 22, AE about 450 nT at 0200 UT Apr 22, more activation of 1500 nT with SYM-H decrease, Kp =6 at SYM-H min

Storm recovery: several SYM-H enhancements during cloud passage, AE low, Kp below 2, SW and IMF nominal, SYM-H to 0 after cloud passage

-1 0

0

1 0

IMF

Bz,

nT

-5 0 0-4 0 0-3 0 0-2 0 0-1 0 0

Vx,

km

/s

0

4

8

1 2

Psw

, nP

a

04 0 08 0 0

1 2 0 01 6 0 0

AE

, nT

0246

Kp

-1 2 0-8 0-4 0

04 0

SY

M-H

, nT

0 1 2 0 1 2 0 1 2 0 1 2 0 1 2 2 4 A p r 2 1 A p r 2 2 A p r 2 3 A p r 2 4 A p r 2 5

(a)

(b)

(c)

(d)

(e)

(f)

A C E

A C E

A C E

Ring current energy density and total energy calculated from Polar CAMMICE/MICS measurements

Energy density of RC protons j(E, L) – measured flux.

Total proton ring current energy:integrated over RC volume of V=1023 m3 (torus with crossection of 2.5 Re, radius of 5 Re), symmetric, no PA corrections

Previous statistical results:- Before storm: main contribution from 80-200 keV,- Main phase: dominance of 30-80 keV,- Recovery: dominance of 80-200 keV.

Difference for April 21-25, 2001 storm:Smaller values, dominance of 1-30 keV.- Polar orbit evolution, ring current fast crossings at high magnetic latitudes, - underestimate of 80-200 keV

,LE,jEdE2mq2πLw0

,dVLwWV

RC


0

0 .4

0 .8

1 .2

RC

ene

rgy,

1014

J (a)

(b)

P olar C AM M IC E/M IC S

-1 2 0

-8 0

-4 0

0

4 0

SY

M-H

, nT

1 -2 0 0 k eV 1 -3 0 k eV 3 0 -8 0 k eV 8 0 -2 0 0 k eV


Ganushkina et al model description

Drift of protons with 90º±60ºpitch angles, 1st and 2nd invariants = const in time-dependent magnetic and electric fields.

kappa-type initial distribution with the observed parameters (T, n) by LANL MPA at R=7 1900-0500 MLT in the equatorial plane.

Drift velocity as sum of ExB and magnetic (gradient and curvature) drifts:

where E0 and B0 are electric and magnetic fields, p is the particle moment, q is the particle charge, τb is the bounce period, Bm is the magnetic field and mirror point Sm, ds is the element of magnetic field line length.

Changes in distribution function and flux calculations using Liouville’s theorem (conservation of distribution function along dynamic trajectory of particles) taking into account charge-exchange processes with cross section by Janev and Smith, 1993 and number density of neutrals by thermosphere model MSISE 90 (Hedin, 1991)


,0

0

220

000

eIB

bq

p

Bv

BE ,/1

2/1'

dsBsBI m

m

S

S m

kappa-type initial distribution with n and TII and T by LANL MPA;

where n is the particle number density, m is the particle mass, E0 = kB T(1-3/2k) is the distribution peak particle energy, kB = 1.3807*10-23 J/K is the Boltzmann constant, T = 1/3 (TII + 2T), gamma functions computed for k=5.

Time-dependent boundary conditions: - measurements within 4 h around midnight; - values averaged for more than one satellite simultaneously in the region; - linear interpolation of data when no satellite.


,

1

0

12/1

12/3

02

k

kE

E

k

k

kE

mnEf

Ganushkina et al model: Initial boundary conditions for April 21-25, 2001 storm

0 .4

0 .8

1 .2

1 .6

2

2 .4

n, c

m-3

0

4

8

1 2

1 6

TII

, T

, ke

VT II

T

LAN L M PA, n ightside


(a)

(b)

Electric field models:(1) Kp-dependent Volland-Stern convection electric field with observed Kp

is the magnetic local time, 0 = 0 is the offset angle from dawn-dusk meridian;

(2) Boyle et al., 1997 polar cap potential dependent on solar wind and IMF parameters applied to Volland-Stern convection field

IMF is the IMF clock angle.

Ganushkina et al model: Models for electric fields for April 21-25, 2001 storm

EB

B

IMFIMFsw

RR

R

RBV

47.10

,2

sin

2sin1.11101.1

2

324

2

2

0

/0093.0159.01

045.0,2

,sin

E

convection

RkVKpKp

A

AR


Magnetic field models:(1) dipole;

(2) Tsyganenko T89 model parameterized by Kp, Kp observed;

(3) Tsyganenko T01s model with the observed input parameters such as Dst index, solar wind dynamic pressure Psw, IMF By and IMF Bz, functions G1 and G2, which depend on IMF Bz and Vsw and take into account the history of solar wind.

Ganushkina et al model: Models for magnetic fields for April 21-25, 2001 storm


Ganushkina et al model results for April 21-25, 2001 storm : Influence of electric and magnetic field models


No initial distribution in the inner magnetosphere

0

1

2

3

4

1 -2 0 0 k eV1 -3 0 k eV

d ip + V S d ip + B o y le

0

1

2

3

4

3 0 -8 0 k eV8 0 -2 0 0 k eV

d ip + T 8 9 + V S d ip + T 8 9 + B o y le

d ip + T 0 1 s+ V S d ip + T 0 1 s+ B o y le

0

1

2

3

4

Pro

ton

ring

cur

rent

ene

rgy,

1014

J

0

1

2

3

4

Pro

ton

ring

cur

rent

ene

rgy,

1014

J

0

1

2

3

4

0

1

2

3

4

-1 2 0

-8 0

-4 0

0

4 0

SY

M-H

, n

T

-1 2 0

-8 0

-4 0

0

4 0

SY

M-H

, n

T



(a ) (b )

Ganushkina et al model: Electric field pulse model

Time varying fields associated with dipolarization in magnetotail, modeled as an electromagnetic pulse (Li et al., 1998; Sarris et al., 2002): Perturbed fields propagate from tail toward the Earth; Time-dependent Gaussian pulse with azimuthal E; E propagates radially inward at a decreasing velocity; decreases away from midnight.Time-dependent B from the pulse is calculated by Faraday’s law.

In spherical coordinates (r, , ): ,expcosc1EE 2p010

d/ttrvrr ai - location of the pulse maximum, r I determines pulse arrival time

brarv - pulse front velocity, d - width of pulse, c1 , p describe LT dependence of E amplitude, largest at 0,

0aE2a cos1v/Rct - delay of pulse from 0 to other LTs, c2 - delay magnitude,va - longitudinal propagation speed


Ganushkina et al. model: Addition of pulsed electromagnetic field for April 21-25, 2001 storm

0

3 0 0

6 0 0

9 0 0

1 2 0 0

1 5 0 0

1 8 0 0

AE

, nT

1 2 3 4 5 6 7 8 9 1 0

0 4 3 52 .8

0 8 0 53 .0

1 0 0 04 .4

1 3 2 54 .0

1 4 2 06 .0

1 5 4 04 .8

1 7 3 04 .0

1 9 4 55 .6

0 1 3 04 .4

0 6 3 02 .8

0 3 6 9 1 2 1 5 1 8 2 1 0 3 6 9 1 2 1 5 1 8 2 1 2 4 A p ril 2 2 A p ril 2 3 U T


Ganushkina et al model results for April 21-25, 2001 storm : Role of smaller-scale electric fields


No initial distribution in the inner magnetosphere

0

1

2

3

4

1 -2 0 0 k eV1 -3 0 k eV

d ip + V S + p u lses d ip + B o y le+ p u lses

0

1

2

3

4

3 0 -8 0 k eV8 0 -2 0 0 k eV

d ip + T 8 9 + V S + p u lses d ip + T 8 9 + B o y le+ p u lses

d ip + T 0 1 s+ V S + p u lses d ip + T 0 1 s+ B o y le+ p u lse s0

1

2

3

4

Pro

ton

ring

cur

rent

ene

rgy,

1014

J

0

1

2

3

4

Pro

ton

ring

cur

rent

ene

rgy,

1014

J

0

1

2

3

4

0

1

2

3

4

-1 2 0

-8 0

-4 0

0

4 0

SY

M-H

, n

T

-1 2 0

-8 0

-4 0

0

4 0

SY

M-H

, n

T



(a ) (b )

Ganushkina et al model: Initial distribution in the inner magnetosphere

for April 21-23, 2001 storm

Initial energy densitydistribution

Final ED map while tracingwith empty magnetosphere


Available observational data not sufficient to reconstruct the prestorm initial proton distribution in the inner magnetosphere.

As initial distribution - model distribution obtained at the end of Apr 25, 2001 after tracing with empty inner magnetosphere.

Ganushkina et al model results for April 21-25, 2001 storm : Effects on the initial distribution


Initial distribution in the inner magnetosphere

0

1

2

3

4

1 -2 0 0 k eV1 -3 0 k eV

d ip + V S d ip + B o y le

0

1

2

3

4

3 0 -8 0 k eV8 0 -2 0 0 k eV

d ip + T 8 9 + V S d ip + T 8 9 + B o y le

d ip + T 0 1 s+ V S d ip + T 0 1 s+ B o y le0

1

2

3

4

Pro

ton

ring

cur

rent

ene

rgy,

1014

J

0

1

2

3

4

Pro

ton

ring

cur

rent

ene

rgy,

1014

J

0

1

2

3

4

0

1

2

3

4

-1 2 0

-8 0

-4 0

0

4 0

SY

M-H

, n

T

-1 2 0

-8 0

-4 0

0

4 0

SY

M-H

, n

T



(a ) (b )

Ganushkina et al model results for April 21-25, 2001 storm : Effects on the initial distribution and smaller-scale fields


Initial distribution in the inner magnetosphere

0

1

2

3

4

1 -2 0 0 k eV1 -3 0 k eV

d ip + V S + p u lses d ip + B o y le+ p u lses

0

1

2

3

4

3 0 -8 0 k eV8 0 -2 0 0 k eV

d ip + T 8 9 + V S + p u lses d ip + T 8 9 + B o y le+ p u lses

d ip + T 0 1 s+ V S + p u lses d ip + T 0 1 s+ B o y le+ p u lses0

1

2

3

4

Pro

ton

ring

cur

rent

ene

rgy,

1014

J

0

1

2

3

4

Pro

ton

ring

cur

rent

ene

rgy,

1014

J

0

1

2

3

4

0

1

2

3

4

-1 2 0

-8 0

-4 0

0

4 0

SY

M-H

, n

T

-1 2 0

-8 0

-4 0

0

4 0

SY

M-H

, n

T



(a ) (b )

Milillo et al. model description Based on AMPTE/CHEM data of 90 PA H+ fluxes at L=3-9.3 for 1.5-316 keV.

Gives ion distributions as a function of L, energy, MLT.

Functional form of model distribution consists of: (1) Gaussian in L added to a continuum with a Gaussian shape in energy for proton flux at intermediate energies of 5-80 keV – CONVECTION/INJECTION POPULATION (2) Gaussian for high energy population (> 40 keV) – DIFFUSION POPULATION

For April 21-25, 2001 storm LANL MPA data for 3-45 keV and SOPA data for 50-400 keV added.

Set of 6 time-evolving parameters (intensity, energy position and width of two populations) applied to the model, model gives storm evolution of two populations.

Total energy is calculated by integrating energy density.


Liemohn et al. model description


Kinetic ring current-atmosphere interaction model (RAM) - solves the gyration and bounce-averaged Boltzmann equation inside of geostationary orbit; - uses second-order accurate numerical schemes to determine hot ion phase space distribution as a function of time, equatorial plane location, energy, and equatorial pitch angle.

Initial conditions from Sheldon and Hamilton [1993].

Sources specified by LANL MPA and SOPA data across the nightside outer boundary.

Loss mechanisms include - flow of plasma out the dayside outer boundary, - precipitation of particles into the upper atmosphere, - pitch angle scattering and drag from Coulomb collisions (plasmaspheric model of Ober et al. [1997]), - charge exchange with neutral hydrogen geocorona (Rairden et al. [1986]).

Milillo et al., Liemohn et al. and Ganushkina et al. model results for April 21-25, 2001 storm : Comparison


0

4

8

1 2

1 6 to ta lco n v ec te dd iffu sed

-1 2 0

-8 0

-4 0

0

4 0

SY

M-H

, nT


(a)

(b)

0

4

8

1 2

1 6

Rin

g cu

rren

t en

ergy

, 10

14 J

3 -2 0 0 k eV3 -3 0 k e V3 0 -8 0 k eV8 0 -2 0 0 k e V

(c)

(d)

to ta l

0

4

8

1 2

1 6

Rin

g cu

rren

t en

ergy

, 10

14 J c o n v e c ted

0

4

8

1 2

1 6d iffu sed

(e)

d ip + se lf-co n s E

d ip + V S

0

4

8

1 2

1 6

R

ing

curr

ent

ener

gy,

1014

J

0

4

8

1 2

1 6

-1 2 0

-8 0

-4 0

0

4 0

SY

M-H

, n

T

( a )

(b )

(c )


0

1

2

3

4 d ip + V S + p u lses

d ip + T 8 9 + V S + p u lses

d ip + T 0 1 s+ V S + p u lses0

1

2

3

4

Pro

ton

ring

cur

rent

ene

rgy,

1014

J

0

1

2

3

4

-1 2 0

-8 0

-4 0

0

4 0

SY

M-H

, n

T0 1 2 0 1 2 0 1 2 0 1 2 0 1 2 2 4 A p r 2 1 A p r 2 2 A p r 2 3 A p r 2 4 A p r 2 5

1 -2 0 0 k eV1 -3 0 k eV

3 0 -8 0 k eV8 0 -2 0 0 k eV

Modelling of April 21-25, 2001 storm event by three ring current models

All models predict - high-energy protons dominate before the storm, - the low and medium energy protons are rapidly enhanced during the main phase of the storm, - slowly decline in energy content throughout the recovery phase of the storm. - main difference between the models is in the contribution from the high-energy protons during the storm.

Ganushkina model predicts a low contribution from these protons, unless an extra electric field is included to replicate substorm injections.

The Milillo model predicts that the high-energy protons dominate throughout the storm.

The Liemohn model predicts a constant contribution from the high-energy protons during the late recovery phase.

Summary


General Summary


Changing from dipole to more realistic magnetic field decreased the RC energy content by 30%.

Details and strength of convection electric field cause only small changes in time-evolving RC energy content.

Time-dependent and localized electric fields are the only means to provide preferential increase of high-energy particles.

Role of diffused processes is rather small in bringing RC ion during main phase.

Relative contributions from diffusion and convection to RC energy content are equal during recovery phase.

Initial populations in the inner magnetosphere and boundary conditions have significant effects on model results.

Summary: Model results to Dst


Converting peak energy values to magnetic perturbations at the Earth’s surfaceDPS formulation:

B = 3.98 * 10-30 ERC

Ganushkina model, ERC = 4*1014 J, B = 10 nTMilillo and Liemohn models, ERC = 14*1014 J, B = 35 nT

Observations: 100 nT

- Models significantly underestimate the total energy in the ring current region- DPS relation does not account for contributions of other current systems to Dst

Include of acceleration processes into models, which are significant in producing high-energy populations (can affect humans and/or technological systems in space)

Need for realistic electric field models!

References (1)

Boyle, C. B., P. H. Reiff, and M. R. Hairston (1997), Empirical polar cap potentials, J. Geophys. Res., 102, 111-125.Ganushkina, N. Yu., T. I. Pulkkinen, T. Fritz (2005), Role of substorm-associated impulsive electric fields in the ring current development during storms, Ann. Geophys., 23, 579-591.Hedin, A. E. (1991), Extension of the MSIS thermosphere model into the middle and lower atmosphere, J. Geophys. Res., 96, 1159.Janev, R. K. and J. J. Smith (1993), Cross sections for collision processes of hydrogen atoms with electrons, protons, and multiply-charged ions, in: Atomic and Plasma-Material Interaction Data for Fusion, Int. At. Energ. Agency, 4.Li, X., D. N. Baker, M. Temerin, et al. (1998), Simulation of dispersionless injections and drift echoes of energetic electrons associated with substorms, Geophys. Res. Lett., 25, 3763-3766.Liemohn, M. W., J. U. Kozyra, M. F. Thomsen, et al., Dominant role of the asymmetric ring current in producing the stormtime Dst (2001), J. Geophys. Res., 106, 10,883-10,904.


References (2)

Milillo A., S. Orsini, and I. A. Daglis (2001), Empirical model of proton fluxes in the equatorial inner magnetosphere. 1. Development, J. Geophys. Res., 106, 25713-25730.Milillo A., S. Orsini, D. C. Delcourt, A. Mura, S. Massetti, E. De Angelis, and Y. Ebihara (2003), Empirical model of proton fluxes in the equatorial inner magnetosphere: 2. Properties and applications, J. Geophys. Res., 108, doi:10.1029/2002JA009581.Ober, D. M., J. L. Horwitz, and D. L. Gallagher (1997), Formation of density troughs embedded in the outer plasmasphere by subauroral ion drift events, J. Geophys. Res., 102, 14,595.Orsini, S., A. Milillo, A. Mura (2004), modeling of the Inner Magnetospheric Time-Evolving Plasma: an empirical approach based on proton distribution, J. Geophys. Res., 109, A11216, doi: 10.1029/ 2004JA010532.Rairden, R. L., L. A. Frank, and J. D. Craven (1986), Geocoronal imaging with Dynamics Explorer, J. Geophys. Res., 91, 13,613.Sarris, T. E, X. Li, N. Tsaggas, and N. Paschalidis (2002), Modeling energetic particle injections in dynamic pulse fields with varying propagation speeds, J. Geophys. Res., 107, 1033, doi:10.1029/2001JA900166.


References (3)

Sheldon R. B., and D. C. Hamilton (1993), Ion transport and loss in the Earth's quiet ring current 1. Data and standard model, J. Geophys. Res., 98, 13491-13508.Stern, D. P. (1975), The motion of a proton in the equatorial magnetosphere, J. Geophys. Res., 80, 595-599.Tsyganenko, N. A. (1989), A magnetospheric magnetic field model with a warped tail current sheet, Planet. Space Sci., 37, 5-20.Tsyganenko, N. A. (2002a), A model of the near magnetosphere with a dawn-dusk asymmetry: 1. Mathematical structure, J. Geophys. Res., 107, 1179, doi:10.1029/2001JA0002192001.Tsyganenko, N. A. (2002b), A model of the near magnetosphere with a dawn-dusk asymmetry: 2. Parameterization and fitting to observations, J. Geophys. Res., 107, 1176, doi:10.1029/2001JA000220.Volland, H. (1973), A semi-empirical model of large-scale magnetospheric electric field, J. Geophys. Res., 78, 171.Wilken, B. et al. (1992), Magnetospheric ion composition spectrometer onboard the CRRES spacecraft, J. Spacecraft and Rockets, 29, 585.


Contributions to RC energy from protons with different energy ranges: 27 storms’ statistics

0

2 0

4 0

6 0

8 0

1 0 0

0

2 0

4 0

6 0

8 0

1 0 0

0

2 0

4 0

6 0

8 0

1 0 0in itia l p h ase m a in p h ase rec o v e ry p h ase

1 -2 0 k eV 2 0 -8 0 k eV 8 0 -2 0 0 k eV

0

2 0

4 0

6 0

8 0

1 0 0

cont

ribu

tion

to to

tal e

nerg

y ra

nge,

%

6 0 4 0 2 0 0 - 2 0 - 4 0D s t , n T

0

2 0

4 0

6 0

8 0

1 0 02 0

4 0

6 0

8 0

1 0 0

cont

ribu

tion

to to

tal e

nerg

y ra

nge,

%

0 -5 0 -1 0 0 -1 5 0 -2 0 0D st, n T

0

2 0

4 0

6 0

8 0

1 0 00

2 0

4 0

6 0

8 0

1 0 0

cont

ribu

tion

to to

tal e

nerg

y ra

nge,

%

-1 0 0 -5 0 0 5 0D st, n T

0

2 0

4 0

6 0

8 0

1 0 0


Documents

3d European Space Weather Week – November 13-17, 2006, Brussels, Belgium Ring current models: How well can they be applied for space weather modeling purposes?