090094

Stellar coronal abundances display different patterns from those in the photospheres comma with enhancements of elements of low first ionisation potentials openParFIPclosePar. The reasons for this are suspected to be rooted in ponderomotive forces in the stellar atmosphere. For stars with high magnetic activity this coronal abundance patterns is seen inversed openPariFIPclosePar. Interestingly comma for M dwarfs the iFIP pattern is observed across the board however comma only moderately high activity M dwarfs have been probed for coronal abundances so far. Here we propose to measure the coronal abundances of a typical low activity M dwarf in 72 ks. We will probe a crucial coronal temperature range to test if the iFIP pattern persists for M dwarfs of low activity or not.

恒星冕层丰度与光球层丰度呈现迥异的分布模式，表现为低第一电离势（First Ionisation Potential, FIP）元素的丰度增强。目前推测该现象的成因与恒星大气中的有质动力密切相关。对于磁活动剧烈的恒星，其冕层丰度分布模式呈现相反的反FIP（inverse FIP, iFIP）特征。值得注意的是，M型矮星普遍呈现反FIP分布模式，但截至目前，仅对中等偏高磁活动的M型矮星开展过冕层丰度探测研究。本研究拟对一颗典型的低磁活动M型矮星开展时长72千秒的冕层丰度测量。我们将针对关键的冕层温度区间开展探测，以验证低磁活动M型矮星是否同样存在反FIP分布模式。