论文标题
A型恒星周围的新出现的散开行星种群 - 围绕HD围绕HD的长期演变163296
Emerging population of gap-opening planets around type-A stars -- Long-term evolution of the forming planets around HD 163296
论文作者
论文摘要
通过检测到此类磁盘中的多次结构的检测，可以推断出嵌入其原星磁盘中的形成行星的存在。这些怀疑的行星中的大多数是通过当前测量敏感性的直接成像观测而无法检测到的。内部迁移和积聚可能使这些推定的行星可以使用多普勒方法，但是生长和轨道进化的实际程度仍然不受限制。 在HD 163296圆盘中的差距源自新生的行星的前提下，我们调查了在何种情况下以及在何种情况下，开阔的行星可以代表围绕A型恒星检测到的系外行星种群的祖细胞。特别是，我们研究了最终行星质量和轨道参数对磁盘粘度的依赖性。在整个磁盘寿命中，在磁盘分散后，在整个磁盘寿命中模拟了嵌入式行星的演变，将不断发展的磁盘结构和可能的磁盘寿命范围考虑在内。 我们发现，行星的最终配置在很大程度上取决于磁盘的$α$粘度参数，并且较少依赖磁盘寿命和初始行星参数的选择。如果我们假设在HD 163296中的行星演变成形成观察到的A型星的外部球星人群，则需要$ 3.16 \ times 10^{ - 4} \lyseSimα\Lessimα\ Lessimα\ Lessim 10^{ - 3} $的$α$参数，以使disk构成较高的迁移率。取决于未来的直接成像调查是否会发现$ M_ \ Mathrm {pl} \ Lessim 3 M_ \ Mathrm {Jup} $和$ A_ \ Mathrm {pl} \ gtrsim 10 \ mathrm {au} $ the gruend thuseption thuseption thus thusepligh磁盘确实具有宽阔的轨道行星。
The presence of forming planets embedded in their protoplanetary disks has been inferred from the detection of multiring structures in such disks. Most of these suspected planets are undetectable by direct imaging observations at current measurement sensitivities. Inward migration and accretion might make these putative planets accessible to the Doppler method, but the actual extent of growth and orbital evolution remains unconstrained. Under the premise that the gaps in the disk around HD 163296 originate from new-born planets, we investigate if and under which circumstances the gap-opening planets could represent progenitors of the exoplanet population detected around A-type stars. In particular, we study the dependence of final planetary masses and orbital parameters on the viscosity of the disk. The evolution of the embedded planets was simulated throughout the disk lifetime and up to 100 Myr after the dispersal of the disk, taking the evolving disk structure and a likely range of disk lifetimes into account. We find that the final configuration of the planets is largely determined by the $α$ viscosity parameter of the disk and less dependent on the choice for the disk lifetime and the initial planetary parameters. If we assume that planets such as those in HD 163296 evolve to form the observed exoplanet population of A-type stars, a $α$ parameter on the order of $3.16 \times 10^{-4} \lesssim α\lesssim 10^{-3}$ is required for the disks to induce sufficiently high migration rates. Depending on whether or not future direct imaging surveys will uncover a larger number of planets with $m_\mathrm{pl} \lesssim 3 M_\mathrm{Jup}$ and $a_\mathrm{pl} \gtrsim 10 \mathrm{AU}$ we expect the $α$ parameter to be at the lower or upper end of this range, always under the assumption that such disks indeed harbor wide orbit planets.
