A self-consistent field method for galactic dynamics
A self-consistent field method for galactic dynamics
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DOI：
10.1086/171025
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发表时间：
1992-02
期刊：
影响因子：
--
通讯作者：
L. Hernquist;J. Ostriker
中科院分区：
文献类型：
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作者：
L. Hernquist;J. Ostriker
本研究描述了一种演化无碰撞恒星系统的算法，以便研究具有类似R exp 1/4定律的密度分布的系统的演化，仅使用展开式中的几个项。对于截断的等温分布得到了很好的拟合，这使得该方法适用于旋转曲线平坦的星系。在现有的超级计算机上，采用约10exp 6-7的N的计算是直接的，使得具有比直接方法(如树形码)更平滑的场的模拟成为可能。轨道是在给定的静态或含时引力场中找到的；势Phi(r，t)由合成密度Rho(r，t)修正而来。讨论了这项技术可能的科学用途，包括矮小星系的潮汐扰动、球状星系中心质量的绝热增长、现实星系模型中的不稳定性以及星系演化的长期过程。
The present study describes an algorithm for evolving collisionless stellar systems in order to investigate the evolution of systems with density profiles like the R exp 1/4 law, using only a few terms in the expansions. A good fit is obtained for a truncated isothermal distribution, which renders the method appropriate for galaxies with flat rotation curves. Calculations employing N of about 10 exp 6-7 are straightforward on existing supercomputers, making possible simulations having significantly smoother fields than with direct methods such as tree-codes. Orbits are found in a given static or time-dependent gravitational field; the potential, phi(r, t) is revised from the resultant density, rho(r, t). Possible scientific uses of this technique are discussed, including tidal perturbations of dwarf galaxies, the adiabatic growth of central masses in spheroidal galaxies, instabilities in realistic galaxy models, and secular processes in galactic evolution.