论文标题
形成行星的氢重组线光度和 - 可定性
Hydrogen recombination line luminosities and -variability from forming planets
论文作者
论文摘要
我们从1至10个木星质量的行星的三维热热动力学模拟中计算了氢重组线的发光度（H- $α$，Paschen-$β$和Brackett-$γ$）。我们探索了各种缺陷，以估算每个假设边界层积聚的情况下灭绝的线排放。当考虑现实的不熟悉性时，只能使用当前仪器来检测到行星$ \ ge $ 10木星质量的线，这强调了大多数行星中人们无法期望可检测到的排放。这可能解释了从观测结果中形成行星的H-$α$的非常低的检测率。虽然线发射来自形成行星及其圆周磁盘，但我们发现仅由于灭绝而只能检测到磁盘分量。我们也检查了线的可变性，发现较高的质量行星的变化较高。此外，我们首次确定了行星质量与氢重组线的光度之间的参数关系，以及吸积发光度和氢重组线亮度之间的方程。
We calculated hydrogen recombination line luminosities (H-$α$, Paschen-$β$ and Brackett-$γ$) from three dimensional thermo-hydrodynamical simulations of forming planets from 1 to 10 Jupiter-masses. We explored various opacities to estimate the line emissions with extinction in each cases assuming boundary layer accretion. When realistic opacities are considered, only lines from planets $\ge$10 Jupiter-mass can be detected with current instrumentation, highlighting that from most planets one cannot expect detectable emission. This might explain the very low detection rate of H-$α$ from forming planets from observations. While the line emission comes from both the forming planet and its circumplanetary disk, we found that only the disk component could be detected due to extinction. We examined the line variability as well, and found that it is higher for higher mass planets. Furthermore, we determine for the first time, the parametric relationship between the mass of the planet and the luminosity of the hydrogen recombination lines, as well as the equation between the accretion luminosity and hydrogen recombination line luminosities.
