阿帕奇点天文台 (APO)/SMARTS 耀斑星运动观测。I. 从光谱和光度同步观测数据中发现中M矮星耀斑期间色球层线的蓝翼不对称现象

Y. Notsu, Adam F. Kowalski, Hiroyuki Maehara, K. Namekata, Kenji Hamaguchi, T. Enoto, Isaiah I. Tristan, S. Hawley, J. Davenport, Satoshi Honda, K. Ikuta, Shun Inoue, Keiichi Namizaki, D. Nogami, Kazunari Shibata
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摘要

我们对中M矮耀斑星YZ CMi、EV Lac和AD Leo进行了时间分辨同步光学光谱和光度观测。利用阿帕奇角天文台 3.5 米和中小口径研究望远镜系统 1.5 米望远镜在 31 个夜晚进行了光谱观测。在探测到的 41 个耀斑中,有 7 个耀斑的 Hα 线出现了明显的蓝翼不对称现象,耀斑的性质也有不同的对应关系。蓝翼不对称的持续时间从 20 分钟到 2.5 小时不等,其中一个耀斑显示出从蓝翼不对称到红翼不对称的转变。在白光和候选非白光耀斑中都能观测到蓝翼不对称现象。所有这 7 个耀斑的 Hβ 线也显示出蓝翼不对称,但其他色球层线显示蓝翼不对称的种类很多。这 7 个耀斑中的一个还通过软 X 射线光谱进行了观测,这使我们能够估计耀斑磁场和耀斑环的长度。蓝移成分的视线速度范围为-73 到 -122 km s-1。假定蓝移是由突出喷发引起的,向上移动的等离子体质量估计为1015-1019 g,这与耀斑能量和太阳日冕物质抛射(CMEs)预期喷发质量之间的关系大致相同。虽然要理解观测到的各种特性还需要进一步的研究,但假设与太阳爆发的加速机制类似,M-矮星上这些可能的突出喷发可能会演变成CME。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Apache Point Observatory (APO)/SMARTS Flare Star Campaign Observations. I. Blue Wing Asymmetries in Chromospheric Lines during Mid-M-Dwarf Flares from Simultaneous Spectroscopic and Photometric Observation Data
We conducted the time-resolved simultaneous optical spectroscopic and photometric observations of mid-M-dwarf flare stars YZ CMi, EV Lac, and AD Leo. Spectroscopic observations were obtained using Apache Point Observatory 3.5 m and Small and Moderate Aperture Research Telescope System 1.5 m telescopes during 31 nights. Among the 41 detected flares, seven flares showed clear blue wing asymmetries in the Hα line, with various correspondences in flare properties. The duration of the blue wing asymmetries range from 20 minutes to 2.5 hr, including a flare showing the shift from blue to red wing asymmetry. Blue wing asymmetries can be observed during both white-light and candidate non-white-light flares. All of the seven flares showed blue wing asymmetries also in the Hβ line, but there are large varieties on which other chromospheric lines showed blue wing asymmetries. One among the 7 flares was also observed with soft X-ray spectroscopy, which enabled us to estimate the flare magnetic field and length of the flare loop. The line-of-sight velocities of the blueshifted components range from –73 to –122 km s−1. Assuming that the blueshifts were caused by prominence eruptions, the mass of upward-moving plasma was estimated to be 1015–1019 g, which are roughly on the relation between flare energy and erupting mass expected from solar coronal mass ejections (CMEs). Although further investigations are necessary for understanding the observed various properties, these possible prominence eruptions on M-dwarfs could evolve into CMEs, assuming the similar acceleration mechanism with solar eruptions.
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