The Dynamics of Spherical Stellar Systems: III. The Relative Loss of Stars WithDifferent Mass

Abstract

A distribution function that includes a velocity-space anisotropy and that satisfies the Boltzmann equation for both large and small energy is used to calculate the relative rate of stellar mass loss from spherical systems. The calculations are based on the velocity-space flux vector, and do not employ the use of a relaxation time. The loss of stars of different mass at varying distances throughout the system from different spherical models demonstrates the dynanmical importance of the low-mass stars. The stars with mass approximates 1/4 the average stellar mass may leave the system, as a result of distant encounters, from 10 to over 100 times faster than the average stars, depending on the model. The depletion of low luminosity stars in galactic clusters and the distribution of white dwarfs in globular clusters is briefly discussed.