HOW IMPORTANT ARE ELECTRON BEAMS IN DRIVING CHROMOSPHERIC EVAPORATION IN THE 2014 MARCH 29 FLARE?

被引:38
作者
Battaglia, Marina [1 ]
Kleint, Lucia [1 ]
Krucker, Saem [1 ,2 ]
Graham, David [3 ]
机构
[1] Univ Appl Sci & Arts Northwestern Switzerland, Inst Technol 4D, Sch Engn, CH-5210 Windisch, Switzerland
[2] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA
[3] INAF Osservatorio Astrofis Arcetri, Florence, Italy
基金
瑞士国家科学基金会;
关键词
Sun: chromosphere; Sun: flares; Sun: UV radiation; Sun:; X-rays; gamma rays; LOOP RADIATIVE HYDRODYNAMICS; SOLAR-SPECTROSCOPIC-IMAGER; IMAGING SPECTROMETER; X-FLARE; RHESSI; PLASMA; ENERGY; PHASE; FE; DIAGNOSTICS;
D O I
10.1088/0004-637X/813/2/113
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present high spatial resolution observations of chromospheric evaporation in the flare SOL2014-03-29T17:48. Interface Region Imaging Spectrograph observations of the Fe XXI lambda 1354.1 line indicate evaporating plasma at a temperature of 10 MK along the flare ribbon during the flare peak and several minutes into the decay phase with upflow velocities between 30 and 200 km s(-1). Hard X-ray (HXR) footpoints were observed by the Ramaty High Energy Solar Spectroscopic Imager for two minutes during the peak of the flare. Their locations coincided with the locations of the upflows in parts of the southern flare ribbon but the HXR footpoint source preceded the observation of upflows in Fe XXI by 30-75 s. However, in other parts of the southern ribbon and in the northern ribbon, the observed upflows were not coincident with an HXR source in time or space, most prominently during the decay phase. In this case evaporation is likely caused by energy input via a conductive flux that is established between the hot (25 MK) coronal source, which is present during the whole observed time-interval, and the chromosphere. The presented observations suggest that conduction may drive evaporation not only during the decay phase but also during the flare peak. Electron beam heating may only play a role in driving evaporation during the initial phases of the flare.
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页数:8
相关论文
共 45 条
[1]   CHROMOSPHERIC EVAPORATION IN A WELL-OBSERVED COMPACT FLARE [J].
ACTON, LW ;
CANFIELD, RC ;
GUNKLER, TA ;
HUDSON, HS ;
KIPLINGER, AL ;
LEIBACHER, JW .
ASTROPHYSICAL JOURNAL, 1982, 263 (01) :409-&
[2]   EVAPORATIVE COOLING OF FLARE PLASMA [J].
ANTIOCHOS, SK ;
STURROCK, PA .
ASTROPHYSICAL JOURNAL, 1978, 220 (03) :1137-1143
[3]   OBSERVATION OF CHROMOSPHERIC EVAPORATION DURING THE SOLAR MAXIMUM MISSION [J].
ANTONUCCI, E ;
DENNIS, BR .
SOLAR PHYSICS, 1983, 86 (1-2) :67-77
[4]   HARD X-RAY FOOTPOINT SIZES AND POSITIONS AS DIAGNOSTICS OF FLARE ACCELERATED ENERGETIC ELECTRONS IN THE LOW SOLAR ATMOSPHERE [J].
Battaglia, M. ;
Kontar, E. P. .
ASTROPHYSICAL JOURNAL, 2011, 735 (01)
[5]   Observations of conduction driven evaporation in the early rise phase of solar flares [J].
Battaglia, M. ;
Fletcher, L. ;
Benz, A. O. .
ASTRONOMY & ASTROPHYSICS, 2009, 498 (03) :891-900
[6]   A numerical tool for the calculation of non-equilibrium ionisation states in the solar corona and other astrophysical plasma environments [J].
Bradshaw, S. J. .
ASTRONOMY & ASTROPHYSICS, 2009, 502 (01) :409-418
[7]   CONVERSION FROM EXPLOSIVE TO GENTLE CHROMOSPHERIC EVAPORATION DURING A SOLAR FLARE [J].
Brosius, Jeffrey W. .
ASTROPHYSICAL JOURNAL, 2009, 701 (02) :1209-1218
[8]   Extreme-ultraviolet and X-ray spectroscopy of a solar flare loop observed at high time resolution: A case study in chromospheric evaporation [J].
Brosius, JW ;
Phillips, KJH .
ASTROPHYSICAL JOURNAL, 2004, 613 (01) :580-591
[9]   Chromospheric height and density measurements in a solar flare observed with RHESSI - I - Theory [J].
Brown, JC ;
Aschwanden, MJ ;
Kontar, EP .
SOLAR PHYSICS, 2002, 210 (1-2) :373-381
[10]   TRANSPORT PHENOMENA IN A COMPLETELY IONIZED-GAS WITH LARGE TEMPERATURE-GRADIENTS [J].
CAMPBELL, PM .
PHYSICAL REVIEW A, 1984, 30 (01) :365-373