论文标题
原球磁盘的辐射流体动力学模拟：磁盘光蒸发速率的出色质量依赖性
Radiation hydrodynamics simulations of protoplanetary disks: Stellar mass dependence of the disk photoevaporation rate
论文作者
论文摘要
最近的多波长观察结果表明，原星盘的内部部分（PPD）的寿命较短，较重的宿主星。由于高质量恒星周围的PPD被强大的紫外线辐射照射，因此光蒸发可以为观察到的趋势提供解释。我们对PPD的光蒸发进行辐射流体动力学模拟，以$ m_* = 0.5 $ - $ - $ 7.0 m _ {\ odot} $的广泛宿主星质量。我们得出了磁盘质量$ \ dot {m} $，其恒星依赖性为$ \ dot {m} \大约7.30 \ times10^{ - 9} { - 9}（m _ {*}/m _ {\ odot}） $ \ dot {m} $缩放的绝对值，带有所采用的Far-ultraviolet和X射线照明。我们得出表面质量损失率，并为其提供多项式函数。我们还开发了一个半分析模型，该模型很好地再现了派生的质量损失率。估计的内盘寿命随着宿主星质量的增加而降低，与观察趋势一致。因此，我们认为光蒸发是PPD分散恒星质量的主要物理机制，可以解释内部磁盘寿命的观察到的恒星质量依赖性。
Recent multi-wavelength observations suggest that inner parts of protoplanetary disks (PPDs) have shorter lifetimes for heavier host stars. Since PPDs around high-mass stars are irradiated by strong ultra-violet radiation, photoevaporation may provide an explanation for the observed trend. We perform radiation hydrodynamics simulations of photoevaporation of PPDs for a wide range of host star mass of $M_* =0.5$-$7.0 M_{\odot}$. We derive disk mass-loss rate $\dot{M}$, which has strong stellar dependence as $\dot{M} \approx 7.30\times10^{-9}(M_{*}/M_{\odot})^{2}M_{\odot}\rm{yr}^{-1}$. The absolute value of $\dot{M}$ scales with the adopted far-ultraviolet and X-ray luminosities. We derive the surface mass-loss rates and provide polynomial function fits to them. We also develop a semi-analytic model that well reproduces the derived mass-loss rates. The estimated inner disk lifetime decreases as the host star mass increases, in agreement with the observational trend. We thus argue that photoevaporation is a major physical mechanism for PPD dispersal for a wide range of the stellar mass and can account for the observed stellar mass dependence of the inner disk lifetime.
