An Empirical Model for Protostellar Collapse
An Empirical Model for Protostellar Collapse
复制标题
原恒星塌缩的经验模型
DOI：
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发表时间：
2000
期刊：
影响因子：
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通讯作者：
D. Ward
中科院分区：
文献类型：
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作者：
A. Whitworth;D. Ward
我们提出了一个新的解析模型，用于在相对孤立的恒星形成区域中原恒星坍缩的初始条件。该模型是非磁性的，并以类似plummer的径向密度剖面为初始条件。它符合：观测到的恒星前核和0类原恒星的密度分布图；最近在恒星前核心的观测中，在很宽的半径范围内收缩速度大致恒定；以及0级和I级原恒星的寿命和吸积率。然而，该模型非常简单，实际上只有两个自由参数，因此它应该为解释恒星前核心和原恒星的观测以及计算辐射输运和随时间变化的化学提供一个有用的框架。作为一个例子，我们建立了恒星前核心L1544的模型。
We propose a new analytic model for the initial conditions of protostellar collapse in relatively isolated regions of star formation. The model is nonmagnetic and is based on a Plummer-like radial density profile as its initial condition. It fits: the observed density profiles of prestellar cores and class 0 protostars; recent observations in prestellar cores of roughly constant contraction velocities over a wide range of radii; and the lifetimes and accretion rates derived for class 0 and class I protostars. However, the model is very simple, having in effect only two free parameters, so it should provide a useful framework for interpreting observations of prestellar cores and protostars and for calculations of radiation transport and time-dependent chemistry. As an example, we model the prestellar core L1544.
影响因子：
3.2
作者：
V. Mannings;A. Boss;S. Russell
通讯作者：
V. Mannings;A. Boss;S. Russell