Results of an unsuccessful attempt to observe H-alpha emission in the central regions of five globular clusters are used to place realistic upper limits on the H-alpha emission-line surface brightness and ionized-hydrogen mass of the clusters. An attempt is made to describe steady-state gas-flow models constructed for globular clusters with total masses of 100,000 and 1 million solar masses. The analysis assumes a spherically symmetric time-independent gas flow, local availability of the mass and energy of injected material, unprocessed ejected material with a normal He abundance and a heavy-element abundance one-tenth the solar value, and collisional ionization by electrons. The choice of an appropriate rate and energy for mass ejection by stars is discussed, the flow equations are integrated, and the resulting relations between input-gas energy and sonic radius are examined. The emissions predicted by the flow models are compared with observed upper limits for 21-cm, free-free, and H-alpha emission.
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Faulkner et al. (1977) studied this question.