Magnetic topology before a 3B/X1.2 flare and the associated CME

H. Li; B. Schmieder; G. Aulanier; A. Berlicki

doi:10.1017/S1743921306002328

Magnetic topology before a 3B/X1.2 flare and the associated CME

H. Li
, B. Schmieder
, G. Aulanier
, A. Berlicki

Research output: Contribution to journal › Article › peer-review

Abstract

We extrapolated observed photospheric magnetic field before the 3B/X1.2 flare occurred in NOAA 10486 on 2003 October 26. Two magnetic null points exist above the active region, which have no crucial role in triggering the flare, even though enhanced TRACE EUV/UV emission was observed before the main flare due to magnetic reconnection near the lower-altitude null point. We conclude that this flare results from the loss of equilibrium due to persistent flux emergence and photospheric motion, and strong shear. The accompanying fast CME with velocity of ∼ 800 km s^-1 shows quick mass pickup and energy increase in the low corona. Its kinetic energy is always larger than its potential energy.

Original language	English
Pages (from-to)	399-400
Number of pages	2
Journal	Proceedings of the International Astronomical Union
Volume	2
Issue number	233
DOIs	https://doi.org/10.1017/S1743921306002328
Publication status	Published - 1 Mar 2006
Externally published	Yes

Keywords

Sun: UV radiation
Sun: flares
Sun: magnetic field

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10.1017/S1743921306002328

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title = "Magnetic topology before a 3B/X1.2 flare and the associated CME",

abstract = "We extrapolated observed photospheric magnetic field before the 3B/X1.2 flare occurred in NOAA 10486 on 2003 October 26. Two magnetic null points exist above the active region, which have no crucial role in triggering the flare, even though enhanced TRACE EUV/UV emission was observed before the main flare due to magnetic reconnection near the lower-altitude null point. We conclude that this flare results from the loss of equilibrium due to persistent flux emergence and photospheric motion, and strong shear. The accompanying fast CME with velocity of ∼ 800 km s-1 shows quick mass pickup and energy increase in the low corona. Its kinetic energy is always larger than its potential energy.",

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author = "H. Li and B. Schmieder and G. Aulanier and A. Berlicki",

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doi = "10.1017/S1743921306002328",

language = "English",

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T1 - Magnetic topology before a 3B/X1.2 flare and the associated CME

AU - Li, H.

AU - Schmieder, B.

AU - Aulanier, G.

AU - Berlicki, A.

PY - 2006/3/1

Y1 - 2006/3/1

N2 - We extrapolated observed photospheric magnetic field before the 3B/X1.2 flare occurred in NOAA 10486 on 2003 October 26. Two magnetic null points exist above the active region, which have no crucial role in triggering the flare, even though enhanced TRACE EUV/UV emission was observed before the main flare due to magnetic reconnection near the lower-altitude null point. We conclude that this flare results from the loss of equilibrium due to persistent flux emergence and photospheric motion, and strong shear. The accompanying fast CME with velocity of ∼ 800 km s-1 shows quick mass pickup and energy increase in the low corona. Its kinetic energy is always larger than its potential energy.

AB - We extrapolated observed photospheric magnetic field before the 3B/X1.2 flare occurred in NOAA 10486 on 2003 October 26. Two magnetic null points exist above the active region, which have no crucial role in triggering the flare, even though enhanced TRACE EUV/UV emission was observed before the main flare due to magnetic reconnection near the lower-altitude null point. We conclude that this flare results from the loss of equilibrium due to persistent flux emergence and photospheric motion, and strong shear. The accompanying fast CME with velocity of ∼ 800 km s-1 shows quick mass pickup and energy increase in the low corona. Its kinetic energy is always larger than its potential energy.

KW - Sun: UV radiation

KW - Sun: flares

KW - Sun: magnetic field

UR - https://www.scopus.com/pages/publications/33750720009

U2 - 10.1017/S1743921306002328

DO - 10.1017/S1743921306002328

M3 - Article

AN - SCOPUS:33750720009

SN - 1743-9213

VL - 2

SP - 399

EP - 400

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

IS - 233

ER -

Magnetic topology before a 3B/X1.2 flare and the associated CME

Abstract

Keywords

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