论文标题
行星形成和大气进化II的统一模拟II：光蒸发的快速磁盘清除产生低质量的超级诞生大气
Unified simulations of planetary formation and atmospheric evolution II: Rapid disk clearing by photoevaporation yields low-mass super-Earth atmospheres
论文作者
论文摘要
超级货币具有低质量h $ _2 $/HE气氛（通常不到质量的10％）。但是，尚未确定超级地球气氛的起源。我们研究了在超级地球及其大气形成过程中光蒸发通过光蒸发清除的作用。我们在不断考虑光蒸发风和磁驱动的磁盘风中对不断发展的磁盘进行了统一的模拟。对于行星岩心的生长模式，我们考虑了有和没有卵石积聚的行星胚胎生长的两种情况。我们的主要发现总结如下。 （i）由于光蒸发而导致的快速磁盘耗散缩短了大气积聚的时间跨度，从而防止超地球核心积聚大气。 （ii）即使行星岩心在没有卵石积聚的情况下通过胚胎积聚而迅速生长，但由于胚胎积聚的隔离质量很小，因此延迟了失控气体积聚的发作。加上快速磁盘清除，可以避免大气的积聚。 （iii）快速磁盘清除后，许多高分子胚胎可以保留在外轨道中。此后，这种胚胎可能会与超级地点发生碰撞，从而导致积聚大气的有效影响。因此，我们发现具有低质量h $ _2 $/HE气氛的超级收获天然是由N-Body仿真产生的，这些模拟考虑了逼真的磁盘演变。
Super-Earths possess low-mass H$_2$/He atmospheres (typically less than 10% by mass). However, the origins of super-Earth atmospheres have not yet been ascertained. We investigate the role of rapid disk clearing by photoevaporation during the formation of super-Earths and their atmospheres. We perform unified simulations of super-Earth formation and atmospheric evolution in evolving disks that consider both photoevaporative winds and magnetically driven disk winds. For the growth mode of planetary cores, we consider two cases in which planetary embryos grow with and without pebble accretion. Our main findings are summarized as follows. (i) The time span of atmospheric accretion is shortened by rapid disk dissipation due to photoevaporation, which prevents super-Earth cores from accreting massive atmospheres. (ii) Even if planetary cores grow rapidly by embryo accretion in the case without pebble accretion, the onset of runaway gas accretion is delayed because the isolation mass for embryo accretion is small. Together with rapid disk clearing, the accretion of massive atmospheres can be avoided. (iii) After rapid disk clearing, a number of high-eccentricity embryos can remain in outer orbits. Thereafter, such embryos may collide with the super-Earths, leading to efficient impact erosion of accreted atmospheres. We, therefore, find that super-Earths with low-mass H$_2$/He atmospheres are naturally produced by N-body simulations that consider realistic disk evolution.
