Chromospheric activity on the late-type star V1355 Ori using Lijiang 1.8-m and 2.4-m telescopes

作     者：Qing-Feng Pi Li-Yun Zhang Liang Chang Xian-Ming Han Hong-Peng Lu Xi-Liang Zhang Dai-Mei Wang 

作者机构：College of Physics/Department of Physics and AstronomyGuizhou University Key Laboratory for the Structure and Evolution of Celestial ObjectsChinese Academy of Sciences Mingde CollegeGuizhou University Yunnan ObservatoriesChinese Academy of Sciences Dept.of Physics and AstronomyButler University 

出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究（英文版）)

年 卷 期：2016年第16卷第10期

页      面：27-34页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 

基　　金：supported by the Astronomic Joint Fund of the National Natural Science Foundation of China and Chinese Academy of Sciences (U1431114,U1631236,U1631109 and 11263001) science and technology innovation team of Guizhou province(No.20154017) supported by the Natural Science Foundation of Guizhou Province Office of Education(Grant No.2014298) 

主　　题：stars： chromosphere  stars： activity    stars： individual （V1355 Ori） 

摘      要：We obtained new high-resolution spectra using the Lijiang 1.8-m and 2.4-m telescopes to inves- tigate the chromospheric activities of V1355 Ori as indicated in the behaviors of Ca n H＆K, Hγ HT, H/3, Na1 D1, D2, Ha and Ca II infrared triplet （IRT） lines. The observed spectra show obvious emissions above the continuum in Ca II H＆K lines, absorptions in the Hδ, Hγ, H/3 and NaI D1, D2 lines, variable behavior （filled-in absorption, partial emission with a core absorption component or emission above the continuum） in the Ha line, and weak self-reversal emissions in the strong filled-in absorptions of the Ca II IRT lines. We used a spectral subtraction technique to analyze our data. The results show no excess emission in the H6 and H7 lines, very weak excess emissions in the Na I D1, D2 lines, excess emission in the H/3 line, clear excess emission in the Ha line, and excess emissions in the Ca II IRT lines. The value of the ratio of EWs542/EWsa9s is in the range 0.9 to 1.7, which implies that chromospheric activity might have been caused by plage events. The value of the ratio EHδ/EHβ is above 3, indicating that the Balmer lines would arise from prominence-like material. We also found time variations in light curves associated with equiva- lent widths of chromospheric activity lines in the Na I D1, phenomena can be explained by plage events, which are activity indicators. D2, Ca II IRT and Ha lines in particular. These consistent with the behavior of chromospheric