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中文摘要：
与从从头到尾拿的五个太阳耀斑的 RHESSI 数据，我们调查力量变换因素捩琠敨牯 ? 挠湡猠' 咨 A 畦汬? 硥汰楡? 慭祮漠獢牥慶楴湯污映慥畴敲 ? 景猠汯牡映慬敲吗？
英文摘要：
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）.
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