H. Maehara, Y. Notsu, K. Namekata, S. Honda, A. Kowalski, Noriyuki Katoh, T. Ohshima, K. Iida, M. Oeda, K. Murata, M. Yamanaka, K. Takagi, M. Sasada, H. Akitaya, K. Ikuta, Soshi Okamoto, D. Nogami, K. Shibata
{"title":"具有OISTER和TESS的M矮耀斑星YZ的时间分辨光谱和光度测定:非白光耀斑期间H$\\alpha$线的蓝色不对称","authors":"H. Maehara, Y. Notsu, K. Namekata, S. Honda, A. Kowalski, Noriyuki Katoh, T. Ohshima, K. Iida, M. Oeda, K. Murata, M. Yamanaka, K. Takagi, M. Sasada, H. Akitaya, K. Ikuta, Soshi Okamoto, D. Nogami, K. Shibata","doi":"10.5281/ZENODO.4564272","DOIUrl":null,"url":null,"abstract":"In this paper, we present the results from spectroscopic and photometric observations of the M-type flare star YZ CMi in the framework of the Optical and Infrared Synergetic Telescopes for Education and Research (OISTER) collaborations during the Transiting Exoplanet Survey Satellite (TESS) observation period. We detected 145 white-light flares from the TESS light curve and 4 H$\\alpha$ flares from the OISTER observations performed between 2019-01-16 and 2019-01-18. Among them, 3 H$\\alpha$ flares were associated with white-light flares. However, one of them did not show clear brightening in continuum; during this flare, the H$\\alpha$ line exhibited blue-asymmetry which has lasted for $\\sim 60$ min. The line of sight velocity of the blue-shifted component is $-80$ - $-100$ km s$^{-1}$. This suggests that there can be upward flows of chromospheric cool plasma even without detectable red/NIR continuum brightening. By assuming that the blue-asymmetry in H$\\alpha$ line was caused by a prominence eruption on YZ CMi, we estimated the mass and kinetic energy of the upward-moving material to be $10^{16}$ - $10^{18}$ g and $10^{29.5}$ - $10^{31.5}$ erg, respectively. The estimated mass is comparable to expectations from the empirical relation between the flare X-ray energy and mass of upward-moving material for stellar flares and solar CMEs. In contrast, the estimated kinetic energy for the non-white-light flare on YZ CMi is roughly $2$ orders of magnitude smaller than that expected from the relation between flare X-ray energy and kinetic energy for solar CMEs. This could be understood by the difference in the velocity between CMEs and prominence eruptions.","PeriodicalId":8493,"journal":{"name":"arXiv: Solar and Stellar Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.0000,"publicationDate":"2020-09-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"30","resultStr":"{\"title\":\"Time-resolved spectroscopy and photometry of an M dwarf flare star YZ Canis Minoris with OISTER and TESS: Blue asymmetry in H$\\\\alpha$ line during the non-white light flare\",\"authors\":\"H. Maehara, Y. Notsu, K. Namekata, S. Honda, A. Kowalski, Noriyuki Katoh, T. Ohshima, K. Iida, M. Oeda, K. Murata, M. Yamanaka, K. Takagi, M. Sasada, H. Akitaya, K. Ikuta, Soshi Okamoto, D. Nogami, K. Shibata\",\"doi\":\"10.5281/ZENODO.4564272\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"In this paper, we present the results from spectroscopic and photometric observations of the M-type flare star YZ CMi in the framework of the Optical and Infrared Synergetic Telescopes for Education and Research (OISTER) collaborations during the Transiting Exoplanet Survey Satellite (TESS) observation period. We detected 145 white-light flares from the TESS light curve and 4 H$\\\\alpha$ flares from the OISTER observations performed between 2019-01-16 and 2019-01-18. Among them, 3 H$\\\\alpha$ flares were associated with white-light flares. However, one of them did not show clear brightening in continuum; during this flare, the H$\\\\alpha$ line exhibited blue-asymmetry which has lasted for $\\\\sim 60$ min. The line of sight velocity of the blue-shifted component is $-80$ - $-100$ km s$^{-1}$. 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引用次数: 30
摘要
本文介绍了凌日系外行星巡天卫星(TESS)观测期间,在光学和红外教育与研究协同望远镜(OISTER)合作框架下对m型耀斑星YZ CMi的光谱和光度观测结果。我们在2019年01月16日至2019年01月18日的OISTER观测中检测到145个白光耀斑和4个H $\alpha$耀斑。其中,3h $\alpha$耀斑与白光耀斑相关。但其中一个在连续体中没有明显的增亮;在这次耀斑期间,H $\alpha$线表现出蓝色不对称,持续了$\sim 60$分钟。蓝移分量的视线速度为$-80$ - $-100$ km s $^{-1}$。这表明,即使没有可检测到的红色/近红外连续体增亮,色球冷等离子体也可能向上流动。假设H $\alpha$线上的蓝色不对称是由YZ CMi上的日珥喷发引起的,我们估计向上移动的物质的质量和动能分别为$10^{16}$ - $10^{18}$ g和$10^{29.5}$ - $10^{31.5}$ erg。估计的质量与耀斑x射线能量与恒星耀斑和太阳日冕物质向上运动物质质量之间的经验关系的期望相当。相比之下,YZ CMi上的非白光耀斑的估计动能大约比耀斑x射线能量与太阳cme动能之间的关系估计的要小$2$个数量级。这可以通过日冕物质抛射和日珥喷发之间的速度差异来理解。
Time-resolved spectroscopy and photometry of an M dwarf flare star YZ Canis Minoris with OISTER and TESS: Blue asymmetry in H$\alpha$ line during the non-white light flare
In this paper, we present the results from spectroscopic and photometric observations of the M-type flare star YZ CMi in the framework of the Optical and Infrared Synergetic Telescopes for Education and Research (OISTER) collaborations during the Transiting Exoplanet Survey Satellite (TESS) observation period. We detected 145 white-light flares from the TESS light curve and 4 H$\alpha$ flares from the OISTER observations performed between 2019-01-16 and 2019-01-18. Among them, 3 H$\alpha$ flares were associated with white-light flares. However, one of them did not show clear brightening in continuum; during this flare, the H$\alpha$ line exhibited blue-asymmetry which has lasted for $\sim 60$ min. The line of sight velocity of the blue-shifted component is $-80$ - $-100$ km s$^{-1}$. This suggests that there can be upward flows of chromospheric cool plasma even without detectable red/NIR continuum brightening. By assuming that the blue-asymmetry in H$\alpha$ line was caused by a prominence eruption on YZ CMi, we estimated the mass and kinetic energy of the upward-moving material to be $10^{16}$ - $10^{18}$ g and $10^{29.5}$ - $10^{31.5}$ erg, respectively. The estimated mass is comparable to expectations from the empirical relation between the flare X-ray energy and mass of upward-moving material for stellar flares and solar CMEs. In contrast, the estimated kinetic energy for the non-white-light flare on YZ CMi is roughly $2$ orders of magnitude smaller than that expected from the relation between flare X-ray energy and kinetic energy for solar CMEs. This could be understood by the difference in the velocity between CMEs and prominence eruptions.