论文标题
原始磁盘受到插入：一维无关模型，并与Alma观测值进行比较
Protostellar disks subject to infall: a one-dimensional inviscid model and comparison with ALMA observations
论文作者
论文摘要
提出了一种新的一维，无情和垂直整合的磁盘模型，并提出了规定的插入式磁盘模型。使用二阶冲击方案计算流量。其中包括垂直插入，径向径向边界处的径向中心，辐射冷却，出色的辐射以及磁盘表面冲击的加热。选择模拟参数以靶向使用Alma（Atacama大毫米阵列）观察到的L1527 IRS磁盘。 The results give an outer envelope of radial infall and $u_ϕ\propto 1/r$ which encounters a radial shock at $r_\mathrm{shock} \sim 1.5\ \times$ the centrifugal radius ($r_\mathrm{c}$) across which the radial velocity is greatly reduced and the gas temperature rises from a pre-shock value of $\approx 25$ K to在空间薄的区域上使用单独的冲击结构代码计算出的空间薄区域上的$ \约180美元。在$ r_ \ mathrm {c} $中，Azimuthal速度$ u_ϕ $从$ \ propto 1/r $转变到几乎是keplerian。这些结果定性地与最近的Alma观测值一致，这些观察结果表明辐射冲击是升华的，以及从$ U_DASS \ SIM 1/R $区域到Keplerian Inner Disk的过渡。但是，在一组观测值中，环状C $ _3 $ h $ _2 $的位置 - 速度图以及一定的弹道最大速度关系，表明径向冲击与弹道中心障碍屏障一致$ r_ \ mathrm {c} $，而不是我们的模拟给出。有人认为，来自先前磁旋转偏移模拟的径向速度图还表明，径向冲击位于$ r_ \ mathrm {c} $的外部。分析和讨论了与观测值的差异，但仍未解决。
A new one-dimensional, inviscid, and vertically integrated disk model with prescribed infall is presented. The flow is computed using a second-order shock-capturing scheme. Included are vertical infall, radial infall at the outer radial boundary, radiative cooling, stellar irradiation, and heat addition at the disk-surface shock. Simulation parameters are chosen to target the L1527 IRS disk which has been observed using ALMA (Atacama Large Millimeter Array). The results give an outer envelope of radial infall and $u_ϕ\propto 1/r$ which encounters a radial shock at $r_\mathrm{shock} \sim 1.5\ \times$ the centrifugal radius ($r_\mathrm{c}$) across which the radial velocity is greatly reduced and the gas temperature rises from a pre-shock value of $\approx 25$ K to $\approx 180$ K over a spatially thin region calculated using a separate shock structure code. At $r_\mathrm{c}$, the azimuthal velocity $u_ϕ$ transitions from being $\propto 1/r$ to being nearly Keplerian. These results qualitatively agree with recent ALMA observations which indicate a radial shock where SO is sublimated as well as a transition from a $u_ϕ\sim 1/r$ region to a Keplerian inner disk. However, in one set of observations, the position-velocity map of cyclic-C$_3$H$_2$, together with a certain ballistic maximum velocity relation, has suggested that the radial shock coincides with a ballistic centrifugal barrier, which places the shock at $r_\mathrm{shock} = 0.5 r_\mathrm{c}$, i.e, inward of $r_\mathrm{c}$, rather than outward as given by our simulations. It is argued that radial velocity plots from previous magnetic rotating-collapse simulations also indicate that the radial shock is located outward of $r_\mathrm{c}$. The discrepancy with observations is analyzed and discussed, but remains unresolved.
