The outer atmospheres of cool M dwarfs

冷 M 矮星的外层大气

• 批准号: 397701660
• 负责人: Professor Dr. Jürgen H.M.M. Schmitt
• 金额: --
• 依托单位: Hamburger Sternwarte
• 依托单位国家: 德国
• 项目类别: Research Grants
• 财政年份: 2018
• 资助国家: 德国
• 起止时间: 2017-12-31 至 2020-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/397701660?language=en
• 关键词: outer; atmospheres; cool; dwarfs

M dwarfs are known to exhibit vastly different levels of magnetic activity, manifesting itself in star spots, X-ray emission and - at optical wavebands - chromospheric emission lines. In order to better understand the physics of these heated outer atmospheric layers for different spectral sub-types and activity levels among M dwarfs, we propose to perform 1D and 3D chromospheric modeling for these stars in the framework of this funding application. We specifically propose to compute both 3D chromospheric models and 1D chromospheric models and check, if the atmospheric inhomogeneities can be accounted for by single or linear combinations of 1D models, and juxtapose this modeling with state-of-the-art observations obtained by CARMENES. We therefore propose to use the atmosphere code PHOENIX for constructing a model grid of classical 1D chromospheres for M dwarfs and confront our modeling with high-resolution spectral observations taken with the CARMENES spectrograph. For selected objects we propose to perform a detailed comparison between observed and modeled spectra to better characterize the physics of the chromospheres of the selected individual stars.

已知M矮人表现出巨大不同的磁性活性，表现在恒星斑点，X射线发射和 - 在光波段中 - 色球发射线。 为了更好地了解这些加热的外部大气层的物理，用于不同光谱子类型和M矮人之间的活性水平，我们建议在此资助应用程序的框架内对这些恒星进行1D和3D色球层建模。 我们特别建议计算3D色球模型和1D色层模型，并检查是否可以通过1D模型的单个或线性组合来考虑大气中的不均匀性，并与Carmenes获得的最先进的观测值并置与最先进的观测值。 因此，我们建议使用大气代码凤凰为M矮人的经典1D色球环的模型网格，并与使用Carmenes光谱仪进行的高分辨率光谱观察结果面对我们的建模。 对于选定的对象，我们建议在观察到的光谱和建模光谱之间进行详细的比较，以更好地表征所选个体恒星的色球球体的物理学。