等温和绝热极限下的绕行星盘动力学
Circumplanetary Disk Dynamics in the Isothermal and Adiabatic Limits
摘要：
环行星盘（CPD）可能对行星的形成至关重要，调节它们的旋转和吸积演化。我们进行了一系列的三维流体动力学模拟在等温和绝热限制系统地测量旋转速率，大小和质量的CPD作为$q_{\rm thermal}$的函数，行星质量的磁盘热质量的比率。我们的$q_{\rm thermal}$范围从0.1到4;对于我们的各种磁盘温度，这对应于1个地球质量和4个木星质量之间的行星质量。在这个参数空间内，我们发现，等温CPD是disky和约束在$\sim$ 10\%的行星的邦迪半径$r_{\rm B}$，与最里面的$\sim0.05\,r_{\rm B}$在充分的旋转支持。绝热CPD是球形的（因此实际上不是“盘”），在$\sim0.2\,r_{\rm B}$内被束缚，并且主要是压力支持的，旋转速率与$q_{\rm thermal}$成线性比例;外推法表明在$\sim10\,q_{\rm thermal}$处绝热包络完全旋转支持。快速旋转和三维超音速流呈现等温CPD显着不同的结构--和数量级小于-他们的一维等温流体静力学同行。在最小质量的太阳星云内，即使是最大冷却的，围绕10个地球质量核心的等温CPD也可能小于1个地球质量，这表明气体巨星的形成可能取决于CPD中的角动量传输过程。我们的CPD的大小和质量似乎与绕太阳系巨星运行的常规卫星一致。
英文摘要：
Circumplanetary disks (CPDs) may be essential to the formation of planets, regulating their spin and accretion evolution. We perform a series of 3D hydrodynamics simulations in both the isothermal and adiabatic limits to systematically measure the rotation rates, sizes, and masses of CPDs as functions of $q_{\rm thermal}$, the ratio of the planet mass to the disk thermal mass. Our $q_{\rm thermal}$ ranges from 0.1 to 4; for our various disk temperatures, this corresponds to planet masses between 1 Earth mass and 4 Jupiter masses. Within this parameter space, we find that isothermal CPDs are disky and bound within $\sim$10\% of the planet's Bondi radius $r_{\rm B}$, with the innermost $\sim0.05\,r_{\rm B}$ in full rotational support. Adiabatic CPDs are spherical (therefore not actually "disks"), bound within $\sim0.2\,r_{\rm B}$, and mainly pressure-supported with rotation rates scaling linearly with $q_{\rm thermal}$; extrapolation suggests full rotational support of adiabatic envelopes at $\sim10\,q_{\rm thermal}$. Fast rotation and 3D supersonic flow render isothermal CPDs significantly different in structure from --- and orders of magnitude less massive than --- their 1D isothermal hydrostatic counterparts. Inside a minimum-mass solar nebula, even a maximally cooled, isothermal CPD around a 10 Earth-mass core may have less than 1 Earth mass, suggesting that gas giant formation may hinge on angular momentum transport processes in CPDs. Our CPD sizes and masses appear consistent with the regular satellites orbiting solar system giants.
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