arXiv 1301.02552013-01-02astro-ph.GAastro-ph.COgr-qc

矮球状星系中波动暗物质的模拟

Modeling Wave Dark Matter in Dwarf Spheroidal Galaxies

Hubert L. Bray, Alan R. Parry

备注：: 22 pages, 10 figures, 3 tables

摘要：

本文研究了一种称为波暗物质（也称为标量场暗物质和玻色子星）的暗物质模型，该模型最近也受到了Bray [arXiv：1212.5745]的新几何视角的启发。波暗物质将暗物质描述为满足Einstein-Klein-Gordon方程的标量场。这些方程依赖于一个基本常数Uppermum（也称为克莱因-戈登方程的“质量项”）。在这项工作中，我们比较波暗物质模型的观测，以获得一个工作值的Upperdance。具体来说，我们比较了波暗物质的球对称静态的质量分布的Burkert质量分布，已被Salucci等人。[arXiv：1111.1165]预测以及八个经典矮球状星系的速度色散分布。我们证明了波动暗物质模型中基本常数的合理工作值是Upperdance = 50 yr^{-1}。我们还表明，在精确的假设下，地球剧变的值可以在1000年^{-1}以上。

英文摘要：

This paper studies a model of dark matter called wave dark matter (also known as scalar field dark matter and boson stars) which has recently also been motivated by a new geometric perspective by Bray [arXiv:1212.5745]. Wave dark matter describes dark matter as a scalar field which satisfies the Einstein-Klein-Gordon equations. These equations rely on a fundamental constant Upsilon (also known as the "mass term" of the Klein-Gordon equation). In this work, we compare the wave dark matter model to observations to obtain a working value of Upsilon. Specifically, we compare the mass profiles of spherically symmetric static states of wave dark matter to the Burkert mass profiles that have been shown by Salucci et al. [arXiv:1111.1165] to predict well the velocity dispersion profiles of the eight classical dwarf spheroidal galaxies. We show that a reasonable working value for the fundamental constant in the wave dark matter model is Upsilon = 50 yr^{-1}. We also show that under precise assumptions the value of Upsilon can be bounded above by 1000 yr^{-1}.

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