Can the temperature of Ellerman Bombs be more than 10 000 K？  

作　　者：Cheng Fang Qi Hao Ming-De Ding Zhen Li 

机构地区：[1]School of Astronomy and Space Science,Nanjing University,Nanjing 210093,China [2]key laboratory of modern astronomy and astrophysics(nanjing university),ministry of education [3]collaborative innovation center of modern astronomy and space exploration

出　　处：《Research in Astronomy and Astrophysics》2017年第4期1-6,共6页天文和天体物理学研究（英文版）

基　　金：supported by the National Natural Science Foundation of China(NSFC,Grant Nos.11533005,11025314,13001003,11203014 and 11103075);NKBRSF(Grant 2014CB744203)

摘　　要：Ellerman bombs （EBs） are small brightening events in the solar lower atmosphere. By their original definition, the main characteristic of EBs is the two emission bumps in both wings of chro- mospheric lines, such as Hα and Ca II 8542A lines. Up to now, most authors have found that the temperature increase of EBs around the temperature minimum region is in the range of 600-3000 K. However, with recent IRIS observations, some authors proposed that the temperature increase of EBs could be more than 10 000 K. Using non-LTE semi-empirical modeling, we investigate the line profiles, continuum emission and radiative losses for EB models with different temperature increases, and com- pare them with observations. Our result indicates that if the EB maximum temperature reaches more than 10000K around the temperature minimum region, then the resulting Hα and Call 8542A line profiles and the continuum emission would be much stronger than those of EB observations. Moreover, due to the high radiative losses, a high temperature EB compatible with observations. Thus, our study does not higher than 10 000 K. would have a very short lifetime, which is not support the proposal that EB temperatures are higher than 10 000 K.Ellerman bombs （EBs） are small brightening events in the solar lower atmosphere. By their original definition, the main characteristic of EBs is the two emission bumps in both wings of chro- mospheric lines, such as Hα and Ca II 8542A lines. Up to now, most authors have found that the temperature increase of EBs around the temperature minimum region is in the range of 600-3000 K. However, with recent IRIS observations, some authors proposed that the temperature increase of EBs could be more than 10 000 K. Using non-LTE semi-empirical modeling, we investigate the line profiles, continuum emission and radiative losses for EB models with different temperature increases, and com- pare them with observations. Our result indicates that if the EB maximum temperature reaches more than 10000K around the temperature minimum region, then the resulting Hα and Call 8542A line profiles and the continuum emission would be much stronger than those of EB observations. Moreover, due to the high radiative losses, a high temperature EB compatible with observations. Thus, our study does not higher than 10 000 K. would have a very short lifetime, which is not support the proposal that EB temperatures are higher than 10 000 K.

关 键 词：line profiles -- Sun： photosphere -- Sun： chromosphere 

分 类 号：P182[天文地球—天文学]