arXiv 1303.26552013-03-11astro-ph.EP

环双星原行星盘中的冰线

Ice Lines in Circumbinary Protoplanetary Disks

Christian Clanton

备注：: 5 pages, 3 figures. Submitted to ApJL
DOI：: 10.1088/2041-8205/768/1/L15

摘要：

我检查的位置的冰线在circumbinary磁盘加热稳定的质量吸积和恒星辐射和比较的临界半长轴，内部的行星轨道是不稳定的。对于给定的双星系统，存在一个临界双星分离点，该分离点的冰线位于临界半长轴内，这取决于双星参数和星盘性质。对于由1 M $_{\odot}$组成的等质量双星，这个临界距离是$\approx 1.04 $ AU，并且与质量吸积率和Rosseland平均不透明度（$\propto [\dot{M}κ_R]^{2/9}$）呈弱比例关系。假设一个稳定的质量吸积率为$\dot{M} \sim 10^{-8} {\rm M_{\odot} yr^{-1}}$和一个Rosseland平均不透明度的$κ_R\sim 1 {\rm cm^2 g^{-1}}$，我表明，$\gtrsim 80%$的所有二元系统的总质量$M_{\rm tot} \lesssim 4.0 M_{\odot}$有冰线，位于内部的临界半长轴。这表明这些系统中不应该形成岩石行星，这一预测可以通过寻找双星周围的行星来验证，这些双星的分离大于\emph{Kepler}（困难）和微透镜的临界分离。

英文摘要：

I examine the position of the ice line in circumbinary disks heated by steady mass accretion and stellar irradiation and compare with the critical semi-major axis, interior to which planetary orbits are unstable. There is a critical binary separation, dependent on the binary parameters and disk properties, for which the ice line lies within the critical semi-major axis for a given binary system. For an equal mass binary comprised of 1 M$_{\odot}$ components, this critical separation is $\approx 1.04 $AU, and scales weakly with mass accretion rate and Rosseland mean opacity ($\propto [\dot{M}κ_R]^{2/9}$). Assuming a steady mass accretion rate of $\dot{M} \sim 10^{-8} {\rm M_{\odot} yr^{-1}}$ and a Rosseland mean opacity of $κ_R\sim 1 {\rm cm^2 g^{-1}}$, I show that $\gtrsim 80%$ of all binary systems with total masses $M_{\rm tot} \lesssim 4.0 M_{\odot}$ have ice lines that lie interior to the critical semi-major axis. This suggests that rocky planets should not form in these systems, a prediction which can be tested by looking for planets around binaries with separations larger than the critical separation with \emph{Kepler} (difficult) and with microlensing.

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英文摘要：

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