Sources of Quasi-periodic Pulses in the Flare of 18 August 2012

被引:5
作者
Altyntsev, A. [1 ]
Meshalkina, N. [1 ]
Meszarosova, H. [2 ]
Karlicky, M. [2 ]
Palshin, V. [3 ]
Lesovoi, S. [1 ]
机构
[1] RAS, SB, Inst Solar Terr Phys, Lermontov St 126A, Irkutsk 664033, Russia
[2] Acad Sci Czech Republ, Inst Astron, CS-25165 Ondrejov, Czech Republic
[3] AF Ioffe Phys Tech Inst, Politekhnicheskaya 26, St Petersburg 194021, Russia
关键词
Radio emission; active regions; Oscillations; solar; X-Ray bursts; association with flares; HARD X-RAY; IMPULSIVE SOLAR-FLARES; ENERGETIC ELECTRONS; RADIO PULSATIONS; LOOP COALESCENCE; EMISSION; ACCELERATION; CONFIGURATION; RECONNECTION; OSCILLATIONS;
D O I
10.1007/s11207-016-0846-9
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We analyzed spatial and spectral characteristics of quasi-periodic pulses (QPP) for the limb flare on 18 August 2012, using new data from a complex of spectral and imaging instruments developed by the Siberian Solar Radio Telescope team and the Wind/Konus -ray spectrometer. A sequence of broadband pulses with periods of approximately ten seconds were observed in X-rays at energies between 25 keV and 300 keV, and in microwaves at frequencies from a few GHz up to 34 GHz during an interval of one minute. The QPP X-ray source was located slightly above the limb where the southern legs of large and small EUV loop systems were close to each other. Before the QPPs occurred, the soft X-ray emission and the Ramaty High Energy Solar Spectroscopic Imager signal from the energy channels below 25 keV were gradually arising for several minutes at the same location. It was found that each X-ray pulse showed a soft-hard-soft behavior. The 17 and 34 GHz microwave sources were at the footpoints of the small loop system, the source emitting in the 4.2 -aEuro parts per thousand 7.4 GHz band in the large system. The QPPs were probably generated by modulated acceleration processes in the energy-release site. We determined the plasma parameters in the radio sources by analyzing the spectra. The microwave pulses might be explained by relatively weak variations of the spectral hardness of the emitting electrons.
引用
收藏
页码:445 / 463
页数:19
相关论文
共 52 条
[1]   THERMAL TO NONTHERMAL ENERGY PARTITION AT THE EARLY RISE PHASE OF SOLAR FLARES [J].
Altyntsev, Alexander A. ;
Fleishman, Gregory D. ;
Lesovoi, Sergey V. ;
Meshalkina, Nataliia S. .
ASTROPHYSICAL JOURNAL, 2012, 758 (02)
[2]   On the microwave spike emission of the September 6, 1992 flare [J].
Altyntsev, AT ;
Grechnev, VV ;
Hanaoka, Y .
SOLAR PHYSICS, 1998, 178 (01) :137-151
[3]   KONUS-W GAMMA-RAY BURST EXPERIMENT FOR THE GGS WIND SPACECRAFT [J].
APTEKAR, RL ;
FREDERIKS, DD ;
GOLENETSKII, SV ;
ILYNSKII, VN ;
MAZETS, EP ;
PANOV, VN ;
SOKOLOVA, ZJ ;
TEREKHOV, MM ;
SHESHIN, LO ;
CLINE, TL ;
STILWELL, DE .
SPACE SCIENCE REVIEWS, 1995, 71 (1-4) :265-272
[4]   Periodic acceleration of electrons in the 1998 November 10 solar flare [J].
Asai, A ;
Shimojo, M ;
Isobe, H ;
Morimoto, T ;
Yokoyama, T ;
Shibasaki, K ;
Nakajima, H .
ASTROPHYSICAL JOURNAL, 2001, 562 (01) :L103-L106
[5]   THEORY OF RADIO PULSATIONS IN CORONAL LOOPS [J].
ASCHWANDEN, MJ .
SOLAR PHYSICS, 1987, 111 (01) :113-136
[6]   Quadrupolar magnetic reconnection in solar flares.: I.: Three-dimensional geometry inferred from Yohkoh observations [J].
Aschwanden, MJ ;
Kosugi, T ;
Hanaoka, Y ;
Nishio, M ;
Melrose, DB .
ASTROPHYSICAL JOURNAL, 1999, 526 (02) :1026-1045
[7]   TRANSPORT OF ENERGETIC ELECTRONS IN A FULLY IONIZED HYDROGEN PLASMA [J].
BAI, T .
ASTROPHYSICAL JOURNAL, 1982, 259 (01) :341-349
[8]   Radio emission from solar flares [J].
Bastian, TS ;
Benz, AO ;
Gary, DE .
ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS, 1998, 36 :131-188
[9]   Stochastic particle acceleration by helical turbulence in solar flares [J].
Fleishman, Gregory D. ;
Toptygin, Igor N. .
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2013, 429 (03) :2515-2526
[10]   FAST GYROSYNCHROTRON CODES [J].
Fleishman, Gregory D. ;
Kuznetsov, Alexey A. .
ASTROPHYSICAL JOURNAL, 2010, 721 (02) :1127-1141