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Power conversion factor in solar flares 被引量:2

Power conversion factor in solar flares
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摘要 With RHESSI data from five solar flares taken from beginning to end,we investigate the power conversion factorμdefined as the ratio of the time derivative of total thermal energy(ERHESSI+Erad+Econd)and the kinetic power(PRHESSI)of nonthermal electrons.Here, ERHESSI is the computed energy contained in thermal plasmas traced by RHESSI SXRs.Other two contributions(Erad and Econd)to the total energy are the energies lost through radiation and conduction,both of which can be derived from the observational data.If both are not considered,μis only positive before the SXR maximum.However,we find that for each flare studiedμis positive over the whole duration of the soalr flare after taking into account both radiation and conduction.Mean values forμrange from 11.7% to 34.6%for these five events,indicating roughly that about this fraction of the known energy in nonthermal electrons is efficiently transformed into thermal energy from start to end.This fraction is traced by RHESSI SXR observations;the rest is lost.The bulk of the nonthermal energy could heat the plasma low in the atmosphere to drive mass flows(i.e.chromospheric evaporation). With RHESSI data from five solar flares taken from beginning to end, we investigate the power conversion factor kt defined as the ratio of the time derivative of total thermal energy (ERHESSI + Erad + Econd) and the kinetic power (PRHESSI) of nonthermal electrons. Here, EmaESSi is the computed energy contained in thermal plasmas traced by RHESSI SXRs. Other two contributions (Erad and Econd) to the total energy are the energies lost through radiation and conduction, both of which can be derived from the observational data. If both are not considered,/l is only positive before the SXR maximum. However, we find that for each flare studied μ is positive over the whole duration of the soalr flare after taking into account both radiation and conduction. Mean values for μ range from 11.7% to 34.6% for these five events, indicating roughly that about this fraction of the known energy in nonthermal electrons is efficiently transformed into thermal energy from start to end. This fraction is traced by RHESSI SXR observations; the rest is lost. The bulk of the nonthermal energy could heat the plasma low in the atmosphere to drive mass flows (i.e. chromospheric evaporation).
作者 NING ZongJun
出处 《Chinese Science Bulletin》 SCIE CAS 2012年第12期1397-1404,共8页
基金 supported by the National Natural Science Foundation of China(10833007,10973042,11073058,11073006,40804034) National Basic Research Program of China(2011CB811400) Key Laboratory of Dark Matter and Space Astronomy,Chinese Academy of Sciences(2010DP173032)
关键词 太阳耀斑 转换因子 电源 热等离子体 总能量 转换系数 时间导数 非热电子 solar flare, X-ray, thermal energy, nonthermal power
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  • 1ZHANG Donghe, XIAO Zuo & CHANG QingDepartment of Geophysics, Peking University, Beijing 100871, China,Qingdao Research Center, China Research Insitute of Radio-wave Propagation, Qingdao 266071, China,Department of Electronic Engineering, Beijing Universit.The correlation of flare's location on solar disc and the sudden increase of total electron content[J].Chinese Science Bulletin,2002,47(1):82-85. 被引量:8
  • 2陈斌,刘立波,万卫星,宁百齐,丁锋.1996—2003年大耀斑事件引起的TEC突然增强的统计分析[J].空间科学学报,2005,25(1):6-16. 被引量:8
  • 3Rong Li Hua-Ning Wang Han He Yan-Mei Cui Zhan-Le Du.Support Vector Machine combined with K-Nearest Neighbors for Solar Flare Forecasting[J].Chinese Journal of Astronomy and Astrophysics,2007,7(3):441-447. 被引量:10
  • 4Zongjun Ning.Magnetic reconnection rate and spectral index for two double-ribbon flares[J]. Astrophysics and Space Science . 2008 (1-3)
  • 5Zongjun Ning.RHESSI Observations of the Neupert Effect in Three Solar Flares[J]. Solar Physics . 2008 (1)
  • 6R.P. Lin,B.R. Dennis,G.J. Hurford,D.M. Smith,A. Zehnder,P.R. Harvey,D.W. Curtis,D. Pankow,P. Turin,M. Bester,A. Csillaghy,M. Lewis,N. Madden,H.F. van Beek,M. Appleby,T. Raudorf,J. McTiernan,R. Ramaty,E. Schmahl,R. Schwartz,S. Krucker,R. Abiad,T. Quinn,P. Berg,M. Hashii,R. Sterling,R. Jackson,R. Pratt,R.D. Campbell,D. Malone,D. Landis,C.P. Barrington-Leigh,S. Slassi-Sennou,C. Cork,D. Clark,D. Amato,L. Orwig,R. Boyle,I.S. Banks,K. Shirey,A.K. Tolbert,D. Zarro,F. Snow,K. Thomsen,R. Henneck,A. Mchedlishvili,P. Ming,M. Fivian,John Jordan,Richard Wanner,Jerry Crubb,J. Preble,M. Matranga,A. Benz,H. Hudson,R.C. Canfield,G.D. Holman,C. Crannell,T. Kosugi,A.G. Emslie,N. Vilmer,J.C. Brown,C. Johns-Krull,M. Aschwanden,T. Metcalf,A. Conway.The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI)[J]. Solar Physics . 2002 (1-2)
  • 7B.N. Handy,L.W. Acton,C.C. Kankelborg,C.J. Wolfson,D.J. Akin,M.E. Bruner,R. Caravalho,R.C. Catura,R. Chevalier,D.W. Duncan,C.G. Edwards,C.N. Feinstein,S.L. Freeland,F.M. Friedlaender,C.H. Hoffmann,N.E. Hurlburt,B.K. Jurcevich,N.L. Katz,G.A. Kelly,J.R. Lemen,M. Levay,R.W. Lindgren,D.P. Mathur,S.B. Meyer,S.J. Morrison,M.D. Morrison,R.W. Nightingale,T.P. Pope,R.A. Rehse,C.J. Schrijver,R.A. Shine,L. Shing,K.T. Strong,T.D. Tarbell,A.M. Title,D.D. Torgerson,L. Golub,J.A. Bookbinder,D. Caldwell,P.N. Cheimets,W.N. Davis,E.E. Deluca,R.A. McMullen,H.P. Warren,D. Amato,R. Fisher,H. Maldonado,C. Parkinson.The transition region and coronal explorer[J]. Solar Physics . 1999 (2)
  • 8Kahler S,,Meekins J,Kreplin R, et al.Temperature and emission-measure proffles of two solar X-ray ffares. The Astrophysical Journal . 1970
  • 9Hudson H.Differential emission-measure variations and the "Neupert effect". Bull Am Astron Soc . 1991
  • 10Veronig A,,Brown J,Dennis B, et al.Physics of the Neupert effect: Estimates of the effects of source energy, mass trans- port, and geometry using RHESSI and GOES data. The Astrophysical Journal . 2005

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