Gas in globular clusters. II - Time-dependent flow models

Details Gas in globular clusters. II - Time-dependent flow models Gas in globular clusters. II - Time-dependent flow models

Dec 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...218..415v&link_type=abstract

Astrophysical Journal, Part 1, vol. 218, Dec. 1, 1977, p. 415-430.

Astronomy and Astrophysics

Astrophysics

35

Astronomical Models, Gas Flow, Globular Clusters, Interstellar Gas, Stellar Mass Ejection, Time Dependence, Boundary Value Problems, Dynamic Models, Finite Difference Theory, Hydrodynamic Equations, Iterative Solution, Radiant Cooling

Scientific paper

A numerical method is described for solving the time-dependent flow equations of relevance to gas flows in globular clusters. This method involves a modification of Henyey's iteration technique as well as finite-difference approximations for mass, momentum, and energy conservation. As an initial application of the numerical method, a previous study is extended to low gas-input energies in order to determine the fate of gas in clusters of one million solar masses when radiative cooling prevents the occurrence of steady-state outflows. Evolutionary sequences of models are presented for selected values of a parameter corresponding to the energy of the gas ejected by a star itself, and the resulting unsteady winds are shown to be similar to those computed by Mathews and Baker (1971) for elliptical galaxies. The results indicate that accumulation of mostly neutral hydrogen may take place in a region of small dimensions near the center of the most tightly bound globular clusters.

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