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Coronal mass ejection of 15 may 2001: II. coupling of the CME acceleration and the flare energy release (CROSBI ID 113035)

Prilog u časopisu | izvorni znanstveni rad | međunarodna recenzija

Vršnak, Bojan ; Maričić, Darije ; Stanger, Andrew ; Veronig, Astrid Coronal mass ejection of 15 may 2001: II. coupling of the CME acceleration and the flare energy release // Solar physics, 225 (2004), 355-378-x

Podaci o odgovornosti

Vršnak, Bojan ; Maričić, Darije ; Stanger, Andrew ; Veronig, Astrid

engleski

Coronal mass ejection of 15 may 2001: II. coupling of the CME acceleration and the flare energy release

We analyze the relationship between the dynamics of the coronal mass ejection (CME) of 15 May 2001 and the energy release in the associated flare. The flare took place behind the east limb and was disclosed by a growing system of hot soft X-ray (SXR) loops that appeared from behind the limb around the onset of the rapid acceleration of the CME. The highly correlated behavior of the SXR light-curve derivative and the time profile of the CME acceleration reveals an intrinsic relationship between the CME dynamics and the flare energy release. Furthermore, we found that the CME acceleration peak occurs simultaneously with the fastest growth (100~km\, s$^{; ; ; -1}; ; ; $) of X-ray loops, indicating that the reconnection plays an essential role in the eruption. Inspecting the CME/flare morphology we recognized in the Yohkoh-SXT images an oval feature that formed within the rising structure at the onset of the rapid acceleration phase, simultaneously with the appearance of the X-ray loops. The eruptive prominence was imbedded within the lower half of the oval, suggestive of the flux-rope/prominence magnetic configuration. We interpret the observed morphological evolution in terms of the reconnection process in the current sheet that presumably formed below the erupting flux-rope at the onset of the CME acceleration. Measurements of the tip-height of the cusped X-ray loop system and the height of the lower edge of the oval, enable us to trace the stretching of the current sheet. The initial distance between the oval and the loops amounted to 35--40~Mm. In about one hour the inferred length of the current sheet increased to 150--200~Mm, which corresponds to the mean elongation-speed of 35--45~km\, s$^{;-1}; $. The results are discussed in the framework of CME models that include the magnetic reconnection below the erupting flux-rope

Sun: coronal mass ejections; Sun: Flares; MHD

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Podaci o izdanju

225

2004.

355-378-x

objavljeno

0038-0938

Povezanost rada

Fizika

Indeksiranost