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RAPID FORMATION OF SUPER-EARTHS AROUND M DWARF STARS

机译：M DWARF恒星周围超地球的快速形成

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摘要

While the recent microlensing discoveries of super-Earths orbiting two M dwarf stars have been taken as support for the core accretion mechanism of giant planet formation, we show here that these planets could also have been formed by the competing mechanism of disk instability, coupled with photoevaporative loss of their gaseous envelopes by a strong external source of UV radiation, i.e., an O star. M dwarfs that form in regions of future high-mass star formation would then be expected to have super-Earths orbiting at distances of several AU and beyond, while those that form in regions of low-mass star formation would be expected to have gas giants at those distances. Given that most stars are born in the former rather than in the latter regions, M dwarfs should have significantly more super-Earths than gas giants, as seems to be indicated by the microlensing surveys.
机译：虽然最近围绕两颗M矮星运行的超地球微透镜发现被认为是支持巨型行星形成的核心吸积机制的证据，但我们在这里表明，这些行星也可能是由磁盘不稳定性的竞争机制形成的，再加上强烈的外部紫外线辐射源（例如O星）会使其气态包膜发生光蒸发损失。预计在未来高质量恒星形成区域中形成的M矮星将以距几个AU或更远距离的超地球轨道运行，而在低质量恒星形成区域中形成的M矮星将具有天然气巨星。在那些距离。鉴于大多数恒星是在前者而不是在后者地区出生的，因此微缩调查似乎表明，M矮星的超地球应该比气体巨星多得多。

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  • 来源
    《The Astrophysical journal》 |2006年第1pt2期|p.L79-L82|共4页
  • 作者

    Alan P. Boss;

  • 作者单位

    Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, NW, Washington, DC 20015-1305;

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  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类 天文学;
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