Density variation in a star field traversed by a globular cluster

Details Density variation in a star field traversed by a globular cluster Density variation in a star field traversed by a globular cluster

Apr 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975sva....18..573a&link_type=abstract

(Astronomicheskii Zhurnal, vol. 51, Sept.-Oct. 1974, p. 973-979.) Soviet Astronomy, vol. 18, Mar.-Apr. 1975, p. 573-576. Transl

Astronomy and Astrophysics

Astronomy

2

Density Distribution, Globular Clusters, Hydrodynamic Equations, Star Distribution, Stellar Motions, Astronomical Models, Black Holes (Astronomy), Field Theory (Physics), Mass, Partial Differential Equations, Stellar Gravitation

Scientific paper

The hydrodynamic equations of stellar dynamics are used to study the flow around a point mass (M) - a globular cluster - moving through a homogeneous star field at constant velocity (V). A formula is derived for the increment in stellar density projected onto a map surface as compared to the nondisturbed spatial density. A characteristic parameter for this increment is the quantity 2GM divided by V squared. Therefore, knowing the velocity of the globular cluster in relation to the local centroid, it is possible to determine the mass of the cluster, including the mass of a black hole if there is one in its center, on the basis of star counts in the vicinity of the cluster.

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