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Higher blueshift components in higher-resolution Fe XXV line profiles as evidence of a time-dependent Petschek-type reconnection
Lin J(林隽); Martin, R; Wu, N; Lin, J
发表期刊ASTRONOMY & ASTROPHYSICS
1996-07
卷号311期号:3页码:1015-1023
产权排序第1完成单位
收录类别SCI
关键词Sun Flares Sun X-rays Sun Magnetic Fields
摘要We re-investigated the higher blueshift components in higher-resolution Fe XXV line profiles observed during some flares by Antonucci et al. (1990a, b) in detail. The present work was mainly concentrated on the initial part of impulsive phase of the 1984 April 24 flare. The results show that the traditional chromospheric evaporation interpretation seems hardly to be able to account for these higher blueshift components. We tried to ascribe these features to the time-dependent Petschek-type reconnection process. On this basis, some important parameters, such as electron density, temperature, magnetic field in the flare region, etc., were estimated. Our results were found reasonable and consistent with the observations and theoretical estimates obtained by others.
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0004-6361
URL查看原文
WOS记录号WOS:A1996UZ29300034
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]X-RAY-SPECTRA ; SOLAR-FLARE TEMPERATURES ; IMPULSIVE PHASE ; CHROMOSPHERIC EVAPORATION ; NUMERICAL SIMULATIONS ; SOFT ; TURBULENCE ; EMISSION ; PLASMA
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被引频次:1[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/6021
专题太阳物理研究组
通讯作者Lin, J
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Lin J,Martin, R,Wu, N,et al. Higher blueshift components in higher-resolution Fe XXV line profiles as evidence of a time-dependent Petschek-type reconnection[J]. ASTRONOMY & ASTROPHYSICS,1996,311(3):1015-1023.
APA 林隽,Martin, R,Wu, N,&Lin, J.(1996).Higher blueshift components in higher-resolution Fe XXV line profiles as evidence of a time-dependent Petschek-type reconnection.ASTRONOMY & ASTROPHYSICS,311(3),1015-1023.
MLA 林隽,et al."Higher blueshift components in higher-resolution Fe XXV line profiles as evidence of a time-dependent Petschek-type reconnection".ASTRONOMY & ASTROPHYSICS 311.3(1996):1015-1023.
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