Abstract
The flow of gas injected from stars in globular clusters is numerically studied by means of the time-dependent beam scheme. By using structural parameters derived by Peterson and King (1975) and taking radiative cooling and ultraviolet heating into account, we obtain the time variation of velocity, temperature and density distributions in the gas flows in nine globular clusters. Flow in NGC 7078 for the specific mass loss rate of 5.34 X w- sec·' is inward within a stagnation point and is outward outside it after a steady state is realized. As the mass loss rate increases, the velocity of the inward flow increases because of the increase in effective cooling. In the clusters with large gravitational fields, gas becomes partial flow as well as in NGC 7078. However, gas flows wholly outwardly in the clusters with weak fields, and heating causes the increase of the velocity of outflow. From the comparison of the cooling time with flow time, it is suggested that the partial inflow is expected in clusters with the gravitational potential of the cluster core greater than 1.0 X 10 12 erg g·'. The gas content in the clusters is also compared with observed data.
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