宇宙氢与冰损失线
Cosmic Hydrogen and Ice Loss Lines
AI总结：
本文通过氢逃逸机制和H₂分解化学平衡计算，在系外行星质量-半径图中提出两条宇宙氢与冰损失线，解释行星原始氢包层随宿主恒星辐射逐渐损失的趋势。
摘要：
我们利用氢及相关挥发物的逃逸机制，以及分子氢（H$_2$）分解为原子氢（H）的化学平衡计算，解释了系外行星质量-半径图中整体依赖于平衡温度的趋势。我们在质量-半径图中确定了两条宇宙氢与冰损失线（CHILLs）。众所周知，气体盘会在一千万年内消散。然而，富含气体的行星可能会在长得多的时间尺度上失去部分或几乎全部气体。因此，我们假设大多数诞生于以氢气为主的原行星盘中的行星，最初都拥有原始H$_2$包层。该包层由于宿主恒星辐射引起的逃逸过程而逐渐损失。
英文摘要：
We explain the overall equilibrium-temperature-dependent trend in the exoplanet mass-radius diagram, using the escape mechanisms of hydrogen and relevant volatiles, and the chemical equilibrium calculation of molecular hydrogen (H$_2$) break-up into atomic hydrogen (H). We identify two Cosmic Hydrogen and Ice Loss Lines (CHILLs) in the mass-radius diagram. Gas disks are well known to disperse in ten million years. However, gas-rich planets may lose some or almost all gas on a much longer timescale. We thus hypothesize that most planets that are born out of a hydrogen-gas-dominated nebular disk begin by possessing a primordial H$_2$-envelope. This envelope is gradually lost due to escape processes caused by host-stellar radiation.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
