PMO OpenIR  > 太阳活动的多波段观测研究团组
Radiative and conductive cooling in a solar flare.PDF
Zongjun Ning ; Dong Li
2011
Source PublicationAstrophysics and Space Science
ISSN1572-946X
Volume338Issue:1Pages:15-21
AbstractWe investigate the radiative and conductive coolingin the solar flare observed by RHESSI on 2005 September13. The radiative and conductive loss energies are estimatedfrom the observations after the flare onset. Consistentwith previous findings, the cooling is increased with time,especially the radiation becomes remarkable on the laterphase of flare. According our method, about half of thermalenergy is traced by RHESSI soft X-rays, while the otherhalf is lost by the radiative (∼38%) and conductive (∼9%)cooling at end of the hard X-rays in this event. The nonthermalenergy input of Pnth (inferred from RHESSI hardX-ray spectrum) is not well correlated with the derivativeof thermal energy of dEthdt (required to radiate the RHESSIsoft X-ray flux and spectrum) alone. However, after considerationthe radiation and conduction, a high correlationis obtained between the derivative of total thermal energy( dEth+Erad+Econddt ) and nonthermal energy input (Pnth) fromthe flare start to end, indicating the relative importance ofconductive and direct radiative losses during the solar flaredevelopment. Ignoring the uncertainties to estimate the energyfrom the observations, we find that about ∼12% fractionof the known energy is transferred into the thermal energyfor the 2005 September 13 flare.
KeywordSun: Flares Sun X-ray Bursts Hard
Subject AreaAstronomy & Astrophysics
Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/4516
Collection太阳活动的多波段观测研究团组
Recommended Citation
GB/T 7714
Zongjun Ning,Dong Li. Radiative and conductive cooling in a solar flare.PDF[J]. Astrophysics and Space Science,2011,338(1):15-21.
APA Zongjun Ning,&Dong Li.(2011).Radiative and conductive cooling in a solar flare.PDF.Astrophysics and Space Science,338(1),15-21.
MLA Zongjun Ning,et al."Radiative and conductive cooling in a solar flare.PDF".Astrophysics and Space Science 338.1(2011):15-21.
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