IMAGING AND SPECTROSCOPIC OBSERVATIONS OF MAGNETIC RECONNECTION AND CHROMOSPHERIC EVAPORATION IN A SOLAR FLARE

被引：120

作者：

Tian, Hui ^{[1
]}

Li, Gang ^{[2
,3
]}

Reeves, Katharine K. ^{[1
]}

Raymond, John C. ^{[1
]}

Guo, Fan ^{[4
]}

Liu, Wei ^{[5
,6
]}

Chen, Bin ^{[1
]}

Murphy, Nicholas A. ^{[1
]}

机构：

[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[2] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA

[3] Univ Alabama, CSPAR, Huntsville, AL 35899 USA

[4] Los Alamos Natl Lab, Los Alamos, NM 87545 USA

[5] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94305 USA

[6] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2014年 / 797卷 / 02期

基金：

美国国家科学基金会;

关键词：

line: profiles; magnetic reconnection; Sun: chromosphere; Sun: flares; Sun: transition region; SUPRA-ARCADE DOWNFLOWS; CURRENT SHEET; PARTICLE-ACCELERATION; TERMINATION SHOCK; HINODE; SPECTROMETER; EJECTIONS; ELECTRONS; DYNAMICS; OUTFLOWS;

D O I：

10.1088/2041-8205/797/2/L14

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Magnetic reconnection is believed to be the dominant energy release mechanism in solar flares. The standard flare model predicts both downward and upward outflow plasmas with speeds close to the coronal Alfven speed. Yet, spectroscopic observations of such outflows, especially the downflows, are extremely rare. With observations of the newly launched Interface Region Imaging Spectrograph (IRIS), we report the detection of a greatly redshifted (similar to 125 km s(-1) along the line of sight) Fe XXI 1354.08.angstrom emission line with a similar to 100 km s(-1) nonthermal width at the reconnection site of a flare. The redshifted Fe XXI feature coincides spatially with the loop-top X-ray source observed by RHESSI. We interpret this large redshift as the signature of downward-moving reconnection outflow/hot retracting loops. Imaging observations from both IRIS and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory also reveal the eruption and reconnection processes. Fast downward-propagating blobs along these loops are also found from cool emission lines (e. g., Si IV, O IV, C II, Mg II) and images of AIA and IRIS. Furthermore, the entire Fe XXI line is blueshifted by similar to 260 km s(-1) at the loop footpoints, where the cool lines mentioned above all exhibit obvious redshift, a result that is consistent with the scenario of chromospheric evaporation induced by downward-propagating nonthermal electrons from the reconnection site.

引用

页数：7

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