Study of a coronal mass ejection using STEREO/SECCHI and SOHO/LASCO observations Alisson Dal Lago 1, Bernd Inhester 2, Luis Eduardo Antunes Vieira 2 1

Study of a coronal mass ejection using STEREO/SECCHI and SOHO/LASCO observations

Alisson Dal Lago1, Bernd Inhester2, Luis Eduardo Antunes Vieira2

1National Institute for Space Research, Sao Jose dos Campos - SP, Brazil2 Max-Planck-Institute for Solar System Research, Katlenburg-Lindau, Germany

► CME on Jan 8-9, 2007. SOHO: LASCO C2 (Jan 8, 2007, at 14:54UT, PA 65);

LASCO C3 (Jan 8-9, 2007) ;STEREO: SECCHI COR1 A&B; SECCHI COR 2 A&B;

SECCHI HI-1 A.

► Solwind – Helios observations

► Estimate of CME travel time to Venus x observations

► Summary

2007/01/08 2007/01/09

Outline

Dal Lago et al., ILWS - 2009

2007/01/08 2007/01/09

Motivation

0 500 1000 1500 2000 2500 3000 35000

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140 LASCO-ACE Solwind-Helios

tr

avel

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e (h

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halo expansion speed (km/s)

Schwenn, Dal Lago, Huttunen (Kilpua) and Gonzalez, Ann. Geophys., 2005


► SOHO: LASCO C2 (Jan 8, 2007, at 14:54UT, PA 65); LASCO C3 (Jan 8-9, 2007) ; EIT (did not detect any activity – CME behind the East limb).

► STEREO: SECCHI COR1 A&B; SECCHI COR 2 A&B; SECCHI HI-1 A.

Set of observations

SECCHI/COR1 B 14:41 UT LASCO/C3 01:42 UT2007/01/08 2007/01/09

The CME on Jan 8-9 2007


STEREO/SECCHI COR 1 B (1.4-4 solar radii) 2007/01/08 14:41 UT

SOHO LASCO C3 (4-32 solar radii) 2007/01/09 02:42 UTSTEREO/SECCHI COR 1 B PA65

SOHO LASCO C3 PA 65

H (

sola

r ra

dii)

Time (h)H

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radi

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Time (h)

5º

5º




STEREO/SECCHI COR 1 B PA65

H (

sola

r ra

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Time (h)

5º



Coronagraph (2 – 18 solar radii) STEREO/SECCHI COR 1 B (1.4-4 solar radii) 2007/01/08 14:41 UT

SOHO LASCO C3 (4-32 solar radii) 2007/01/09 02:42 UT

STEREO/SECCHI COR 1 B PA 65

SOHO LASCO C3 PA 65

H (

sola

r ra

dii)

Time (h)

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time (h)Jan. 8th-9th, 2007

SECCHI COR1B SECCHI COR2B LASCO C3 LASCO C2 SECCHI COR2A SECCHI COR1A LinFit COR1B

Vcor1B = 70.97 km/s Est. onset date/time: 2007/01/08 07:42 UT

LinFit LASCO C3 Vc3 = 283.77 km/s PA 155 deg.


12 14 16 18 20 22 24 26 28 30 32 34 36 38 40 420

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Leading edge of the CME at PA 65 derived from visual detection of the radial intensity profile.

H(s

ola

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SECCHI COR1B SECCHI COR2B LASCO C3 LASCO C2 SECCHI COR2A SECCHI COR1ASECCHI HI1A

SECCHI COR1B Vcor1B = 70.97 km/s Est. onset date/time: 2007/01/08 07:42 UTLASCO C3 Vc3ps = 283.77 km/sSECCHI HI1A Vhi_1a = 345.59 km/s PA 65 deg.

Coronagraph (2 – 40 solar radii)

STEREO/SECCHI COR 1 B PA155

H (

sola

r ra

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Time (h)


STEREO/SECCHI HI-1 A 2007/01/09


Sun Venus

► Coronal Mass Ejection



Sun Venus

Jan 8, 2007



Sun Venus

t1AU = 203 – 20.77*ln(Vexp); (Schwenn et al., 2005) (1)

t1AU (Vexp=260km/s) = 87 hours (2)

T0.72AU = 0.72* t1AU (3) hence, T0.72AU = 63 hours (4)


Vexp

Vrad

Venus1 AU


Sun Venus

Year CME date CME time CME speed (km/s)

ICME date ICME time Helios 1 helioc. Dist. (AU)

Travel time from the Sun (h)

1979 Oct. 10 07:13 170 Oct. 13 02:00 0.72 67 1981 May 8 23:35 1000 May 10 03:20 0.67 27 1981 Jul. 22 20:49 800 Jul. 24 15:28 0.74 43 1981 Nov. 15 00:15 550 Nov. 16 15:19 0.67 39 1982 Nov. 22 20:30 620 Nov. 24 00:01 0.74 27.5

Quadrature observation of CMEs and corresponding ICMEs using SOLWIND coronagraph and Helios 1 plasma analyzer at heliocentric distance of 0.72+ 0.05 AU, from 1979 to 1982 (adapted from Sheeley et al., 1985).

Solwind - Helios


*

Solwind - Helios





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SECCHI COR1B SECCHI COR2B LASCO C3 LASCO C2 SECCHI COR2A SECCHI COR1A LinFit COR1B

Vcor1B = 70.97 km/s Est. onset date/time: 2007/01/08 07:42 UT

LinFit LASCO C3 Vc3 = 283.77 km/s PA 155 deg.

14 15 16 17 18 19 20 21 22 23 24 252

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SECCHI COR2B SECCHI COR2A LASCO C2 PA 65 deg. V = 120 km/s

time (h)

Jan. 8th-9th, 2007

H(s

ola

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Sun Venus

Assumption Travel time to 0.72 AU (hours) Estimated arrival date/time in Venus

comparison with similar past events (Sheeley et al., 1985)

67 Jan. 11th (2007), 09:54 UT

CME travel time model (Schwenn et al., 2005) adapted to 0.72AU

63 Jan. 11th (2007), 05:54 UT

constant final LASCO C3 velocity 105 Jan. 12th (2007), 23:54 UT


Vexp

Vrad

Venus1 AU


► Observed by SOHO’s LASCO C2/C3 and STEREO SECCHI COR1A&B/2A&B and HI1A

► Detailed information was extracted using image processing techniques;

► CME released in the direction of Venus;

► Solwind – Helios comparison

► Various methods to predict travel time to Venus: not successful.

Summary



The authors would like to acknowledge SOHO LASCO and EIT work team and STEREO SECCHI work team for providing the data used in this work. SOHO is a project of international cooperation between ESA and NASA. STEREO SECCHI data are produced by an international consortium of the Naval Research Lab. (US), Lockheed Martin Solar Astrophysics Lab (US), NASA Goddard Space Flight Center (US), Rutherford Appleton Lab (UK), Univ. of Birmingham (UK), Max-Planck-Institut für Sonnensystemforshung (Germany), Centre Spatiale de Liege (Belgium), Institut d’Optique Théorique et Appliqueé (France), and the Institut d’Astrophysique Spatiale (France).A. Dal Lago would like to acknowledge “Conselho Nacional de Desenvolvimento Científico e Tecnologico – CNPq”, of Brazil, for financial support.

Acknowledgements



Documents

Study of a coronal mass ejection using STEREO/SECCHI and SOHO/LASCO observations Alisson Dal Lago 1, Bernd Inhester 2, Luis Eduardo Antunes Vieira 2 1