Globular cluster winds with central accretion by a massive compact object or subcluster

Details Globular cluster winds with central accretion by a massive compact object or subcluster Globular cluster winds with central accretion by a massive compact object or subcluster

May 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981mnras.195..535d&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 195, May 1981, p. 535-551. NASA-supported research.

Astronomy and Astrophysics

Astronomy

10

Globular Clusters, Gravitational Effects, Stellar Mass Accretion, Stellar Winds, Black Holes (Astronomy), Isothermal Processes, Steady State, Stellar Mass Ejection, Stellar Models, White Dwarf Stars

Scientific paper

Steady-state isothermal wind flows are computed with accretion by a central mass concentration in spherically symmetric systems of gas-losing stars. Solutions are uniquely determined by two dimensionless parameters lambda and m, where lambda is approximately equal to the square of the ratio of the central escape velocity to the sound speed and m is approximately equal to the ratio of the central point mass to the cluster core mass. The models are applied to globular clusters for two types of central mass concentration - a single massive black hole and a subcluster of massive stars. A hard (greater than a keV) X-ray source due to a central black hole fed by clusterwide inflow does not provide a consistent model for globular cluster X-ray sources. However, in the case of hot (T being greater than or approximately equal to 2 x 10 to the 5th K) winds, gas trapping by a central subcluster of neutron stars or of binaries containing white dwarfs could explain recent UV and H-alpha observations. Similar applications to elliptical galaxies are discussed.

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