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Coupling between magnetic reconnection, energy release, and particle acceleration in the X17.2 2003 October 28 solar flareстатья
Статья опубликована в высокорейтинговом журнале
Статья опубликована в журнале из списка Web of Science и/или Scopus- Авторы: Kurt Victoria G., Veronig Astrid M., Fleishman Gregory D., Hinterreiter Jürgen, Tschernitz Johannes, Lysenko Alexandra L.
- Журнал: Astronomy and Astrophysics
- Том: 686
- Номер: A195
- Год издания: 2024
- Издательство: Springer Verlag
- Местоположение издательства: Germany
- Первая страница: 195
- Последняя страница: 209
- DOI: 10.1007/s11207-010-9669-2
- Аннотация: Context. The 2003 October 28 (X17.2) eruptive flare was a unique event. The coronal electric field and the pi-decay gamma-ray emissionflux displayed the highest values ever inferred for solar flares.Aims. Our aim is to reveal physical links between the magnetic reconnection process, energy release, and acceleration of electronsand ions to high energies in the chain of the magnetic energy transformations in the impulsive phase of the solar flare.Methods. The global reconnection rate, fi(t), and the local reconnection rate (coronal electric field strength), Ec(r; t), were calculated from flare ribbon separation in Halpha filtergrams and photospheric magnetic field maps. Then, HXRs measured by CORONAS-F/SPRNand the derivative of the GOES SXR flux, ˙ ISXR(t) were used as proxies of the flare energy release evolution. The flare early risephase, main raise phase, and main energy release phase were defined based on temporal profiles of the above proxies. The availableresults of INTEGRAL and CORONAS-F/SONG observations were combined with Konus-Wind data to quantify the time behaviorof electron and proton acceleration. Prompt -ray lines and delayed 2.2MeV line temporal profiles observed with Konus-Wind andINTEGRAL/SPI were used to detect and quantify the nuclei with energies of 1070MeV.Results. The magnetic-reconnection rates, ˙ '(t) and Ec(r; t), follow a common evolutionary pattern with the proxies of the flare energy released into high-energy electrons. The global and local reconnection rates reach their peaks at the end of the main rise phase of the flare. The spectral analysis of the high-energy gamma-ray emission revealed a close association between the acceleration process efficiencythe reconnection rates. High-energy bremsstrahlung continuum and narrow gamma-ray lines were observed in the main rise phase when Ec(r; t) of the positive /(negative) polarity reached values of 120V/cm 80V/cm). In the main energy release phase, the upperenergy of the bremsstrahlung spectrum was significantly reduced and the pion-decay -ray emission appeared abruptly. We discussthe reasons why the change of the acceleration regime occurred along with the large-scale magnetic field restructuration of this flare.Conclusions. The similarities between the proxies of the flare energy release with ˙ pfi(t) and Ec(r; t) in the flare’s main rise phase are in accordance with the reconnection models.We argue that the main energy release and proton acceleration up to subrelativistic energies began just when the reconnection rate was going through the maximum, that is, following a major change of the flare topology.
- Добавил в систему: Курт Виктория Гдальевна
Прикрепленные файлы
| № | Имя | Описание | Имя файла | Размер | Добавлен |
|---|---|---|---|---|---|
| 1. | aa49130-23.pdf | aa49130-23.pdf | 2,2 МБ | 2 сентября 2024 [vlasova] | |
| 2. | Полный текст | aa49130-23_7fKJrQc.pdf | 2,2 МБ | 2 сентября 2024 [vlasova] |