arXiv 0705.01272007-05astro-ph

恒星形成SPH模拟中的辐射转移和能量方程

Radiative transfer and the energy equation in SPH simulations of star formation

D. Stamatellos, A. P. Whitworth, T. Bisbas, S. Goodwin

备注：: Submitted to A&A, recommended for publication
DOI：: 10.1051/0004-6361:20077373

摘要：

我们介绍和测试一种新的和高效的方法来处理热效应和辐射效应影响的能量方程在SPH模拟恒星形成。该方法使用每个粒子的密度，温度和引力势来估计平均光学深度，然后调节粒子的加热和冷却。该方法捕获-在最小的计算成本-的影响（一）的旋转和振动自由度的H2，H2解离，H 0电离，（二）不透明度的变化，由于冰地幔融化，升华的灰尘，分子线，H-，束缚自由和自由自由的过程和电子散射;（四）外部照射;和（五）热惯性。新算法再现了以前的作者和/或已知的解析解的结果。计算成本是一个标准的SPH模拟与一个简单的正压状态方程。该方法易于实现，可以应用于基于粒子和基于网格的代码，并且处理光学深度0<tau<10^{11}。

英文摘要：

We introduce and test a new and highly efficient method for treating the thermal and radiative effects influencing the energy equation in SPH simulations of star formation. The method uses the density, temperature and gravitational potential of each particle to estimate a mean optical depth, which then regulates the particle's heating and cooling. The method captures -- at minimal computational cost -- the effects of (i) the rotational and vibrational degrees of freedom of H2, H2 dissociation, H0 ionisation, (ii) opacity changes due to ice mantle melting, sublimation of dust, molecular lines, H-, bound-free and free-free processes and electron scattering; (iv) external irradiation; and (v) thermal inertia. The new algorithm reproduces the results of previous authors and/or known analytic solutions. The computational cost is comparable to a standard SPH simulation with a simple barotropic equation of state. The method is easy to implement, can be applied to both particle- and grid-based codes, and handles optical depths 0<tau<10^{11}.

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