SIMBAD references

Observations of the intra-cluster medium (ICM) in galactic globular clusters (GCs) show a systematic deficiency in ICM mass as compared to that expected from accumulation of stellar winds in the time available between galactic plane crossings. In this paper, we re-examine the original hypothesis of Scott & Durisen that hydrogen-rich explosions on accreting white dwarfs, classical novae (CNe), will sweep out the ICM from the cluster more frequently than galactic plane crossings. From the CNe rate and stellar mass loss rate, this clearing mechanism predicts that ~0.03 M_☉ should be present in ≤10⁵ M_☉GCs. We model the expanding remnant made from the 10^–4 M_☉ nova ejecta and show that it escapes long before it has cooled. We discuss the few positive ICM measurements and use a Monte Carlo simulation of the accumulation and CNe recurrence times to reveal the possible variance in the ICM masses for the higher-mass (>5x10⁵ M_☉) GCs. We find that nova shells are effective at clearing the ICM in low-mass GCs (≤10⁵ M_☉), whereas higher-mass clusters may experience a quiescent time between novae long enough to prevent the next nova shell from escaping. The nova clearing mechanism will also operate in ultra-faint Milky Way satellites, where many upper limits on gas masses are available.