arXiv 2202.030062022-02-07astro-ph.SR

磁活动M矮星Wolf 359光学耀斑的同时探测

Simultaneous Detection of Optical Flares of the Magnetically Active M Dwarf Wolf 359

Han-Tang Lin, Wen-Ping Chen, Jinzhong Liu, Xuan Zhang, Yu Zhang, Andrew Wang, Shiang-Yu Wang, Matthew J. Lehner, C. Y. Wen, J. K. Guo, Y. H. Chang, M. H. Chang,… 展开作者

Han-Tang Lin, Wen-Ping Chen, Jinzhong Liu, Xuan Zhang, Yu Zhang, Andrew Wang, Shiang-Yu Wang, Matthew J. Lehner, C. Y. Wen, J. K. Guo, Y. H. Chang, M. H. Chang, Anli Tsai, Chia-Lung Lin, C. Y. Hsu, Wing Ip

备注：: 16 pages, 10 figures, 3 tables
DOI：: 10.3847/1538-3881/ac4e92

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摘要：

本文报道了位于太阳附近（2.41秒差距）的M6.5矮星沃尔夫359的耀斑观测结果。观测于2020年4月23日至29日在中国新疆进行，使用1米和0.5米望远镜，相距近300公里。在27小时的光度监测中，共探测到13个光学耀斑，每个耀斑的总能量为$\gtrsim 5 \times 10^{29}$ erg。测得的事件发生率约为每两小时一次，这与之前报道的这颗恒星的无线电，X射线和光学波长一致。4月26日，这两台望远镜都探测到了这样一个耀斑，它是一个释放能量接近$10^{33}$ ~erg的高能事件。在不同的节奏和曝光时间采样的这一重大事件的两个望远镜的光变曲线，使我们能够更好地估计的内在耀斑的轮廓，达到了峰值的恒星静态亮度的1.6倍，否则会被低估的约$0.4$和$0.8$，分别与单望远镜观察到的耀斑振幅。快速采样，以解决耀斑配置文件与更长的积分时间，更高的光度信号噪声之间的折衷提供了一个有用的指导，在未来的耀斑观测的实验设计。

英文摘要：

We present detections of stellar flares of Wolf\,359, an M6.5 dwarf in the solar neighborhood (2.41~pc) known to be prone to flares due to surface magnetic activity. The observations were carried out from 2020 April 23 to 29 with a 1-m and a 0.5-m telescope separated by nearly 300~km in Xinjiang, China. In 27~hr of photometric monitoring, a total of 13 optical flares were detected, each with a total energy of $\gtrsim 5 \times 10^{29}$~erg. The measured event rate of about once every two hours is consistent with those reported previously in radio, X-ray and optical wavelengths for this star. One such flare, detected by both telescopes on 26 April, was an energetic event with a released energy of nearly $10^{33}$~erg. The two-telescope lightcurves of this major event sampled at different cadences and exposure timings enabled us to better estimate the intrinsic flare profile, which reached a peak of up to 1.6 times the stellar quiescent brightness, that otherwise would have been underestimated in the observed flare amplitudes of about $0.4$ and $0.8$, respectively, with single telescopes alone. The compromise between fast sampling so as to resolve a flare profile versus a longer integration time for higher photometric signal-to-noise provides a useful guidance in the experimental design of future flare observations.

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