中晚期M矮星的后退的宇宙海岸线:活跃寿命的测量加剧了岩石系外行星对大气保留的挑战

Emily K. Pass, David Charbonneau and Andrew Vanderburg
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引用次数: 0

摘要

探测和描述类地系外行星的大气层是系外行星天文学的一个关键目标,鉴于即将开展的詹姆斯·韦伯太空望远镜对岩石m矮星世界进行大规模调查,这个目标现在可能触手可及。我们必须了解已知的行星相对于宇宙海岸线的位置,即有大气层和没有大气层的行星之间的界限。先前的研究使用更大质量的恒星校准的比例关系来模拟中晚期M矮星行星接收的历史x射线和紫外线(XUV)辐射,但是完全对流的M矮星显示出与类太阳恒星和早期M矮星不同的独特旋转/活动历史。我们综合了对中晚期M矮星活跃寿命的观测,提出了对它们历史上的XUV影响的最新估计。对于已知的不活跃的中晚期M矮星行星,我们计算了历史上的XUV影响,平均是标准XUV标度关系的2.1-3.1倍,其中较大的值包括主序前阶段和高能耀斑的修正。我们发现,只有已知的最大的类地行星绕中晚期M矮星运行,才可能在宇宙海岸线范式中保留大气层。我们的计算可能有助于指导JWST目标的选择,并可能证明对解释结果有用;为此,我们定义了一种新的大气保留度量(ARM),用于指示行星与宇宙海岸线之间的距离,并将已知中晚期m矮行星的ARM制成表格。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
The Receding Cosmic Shoreline of Mid-to-late M Dwarfs: Measurements of Active Lifetimes Worsen Challenges for Atmosphere Retention by Rocky Exoplanets
Detecting and characterizing the atmospheres of terrestrial exoplanets is a key goal of exoplanetary astronomy, one that may now be within reach given the upcoming campaign to conduct a large-scale survey of rocky M-dwarf worlds with the James Webb Space Telescope. It is imperative that we understand where known planets sit relative to the cosmic shoreline—the boundary between planets that have retained atmospheres and those that have not. Previous works modeled the historic X-ray and ultraviolet (XUV) radiation received by mid-to-late M-dwarf planets using a scaling relation calibrated using more massive stars, but fully convective M dwarfs display unique rotation/activity histories that differ from Sun-like stars and early M dwarfs. We synthesize observations of the active lifetimes of mid-to-late M dwarfs to present an updated estimate of their historic XUV fluence. For known planets of inactive, mid-to-late M dwarfs, we calculate a historic XUV fluence that is 2.1–3.1 times the canonical XUV scaling relation on average, with the larger value including corrections for the pre-main-sequence phase and energetic flares. We find that only the largest terrestrial planets known to orbit mid-to-late M dwarfs are likely to have retained atmospheres within the cosmic shoreline paradigm. Our calculations may help to guide the selection of targets for JWST and may prove useful in interpreting the results; to this end, we define a novel atmosphere retention metric (ARM) that indicates the distance between a planet and the cosmic shoreline, and tabulate the ARM for known mid-to-late M-dwarf planets.
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