Dark matter distribution in the Milky Way

被引：0

作者：

Kalberla, PMW ^{[1
]}

Kerp, JD ^{[1
]}

Haud, U ^{[1
]}

机构：

[1] Univ Bonn, Inst Radioastron, D-53121 Bonn, Germany

来源：

DYNAMICS OF STAR CLUSTERS AND THE MILKY WAY | 2001年 / 228卷

关键词：

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We discuss the hypothesis that the dark matter in the Milky Way may be distributed as a thick isothermal disk. We model the galactic mass distribution on scales R < 50 kpc and derive in a self-consistent way the associated gravitational potential. Our basic assumption is that the shape of the gaseous galactic halo, observable from synchrotron radiation, gamma-rays, soft X-ray background and from Hi lines with high-velocity dispersion needs to be explained by the isothermal mass distribution. For the solar radius R-circle dot=8.5 kpc and a rotation velocity v(circle dot)= 220 kms(-1) we derive a local gravitational acceleration perpendicular to the galactic plane, K-z, and a local surface mass density for \z\ < 1.1 kpc which is in close agreement with recent determinations. Also our Oort Emit of p(circle dot)similar to0.09 M(circle dot)pc(-3) agrees well with recent HIPPARCOS results.

引用

页码：467 / 469

页数：3

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