A round dynamical model of the metal-weak stellar halo

Details A round dynamical model of the metal-weak stellar halo A round dynamical model of the metal-weak stellar halo

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...359..104v&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 359, Aug. 10, 1990, p. 104-111.

Astronomy and Astrophysics

Astrophysics

10

Galactic Structure, Halos, Milky Way Galaxy, Stellar Models, Dark Matter, Dynamic Models, Interstellar Gas

Scientific paper

A dynamical model of the stellar metal-weak halo is constructed using a model of the Galactic potential which represents the Galactic disk in a realistic way. The halo model is a superposition of a Michie-Bodenheimer type phase space distribution and a shell orbit component. The resulting model is quite round with q roughly 0.7 and is characterized by a logarithmic density gradient of roughly -3.4 from the solar circle and beyond. The local value of the anisotropy parameter is roughly 0.6. The kinematic behavior shows isotropy in the central parts, radial dominance at intermediate distances, and tangential dominance at large distances.

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