| Abstract: | The paper analyzes possible origins of stars located in intergalactic space that are not bound to specific galaxies, which
comprise 15–50% of all stars in galaxy clusters. Some such stars can form in streams of intergalactic gas flowing around gas-rich
disk galaxies moving in the cluster. Others may be the products of the decay of young, low-mass, spheroidal galaxies after
the loss of their gaseous components during an initial burst of star formation. The decay of low-mass disk galaxies moving
at high speeds after they have lost their gaseous components due to the pressure of the incident flow of dense intergalactic
gas is possible in the cluster core. The largest fraction of intergalactic stars are probably produced by the partial disruption
of galaxies as a result of close passages, collisions, or mergers. Collisions of low-mass, gas-rich galaxies are especially
good suppliers of intergalactic stars. Both stars from decaying stellar components of galaxies and stars arising in the gaseous
components of colliding galaxies can be supplied to the intergalactic medium. The merger of galaxies harboring supermassive
black holes in their nuclei could lead to the partial or total disruption of these galaxies during the deceleration of the
binary black hole that is formed during the merger. An enhanced density of intergalactic stars is observed in the cores of
galaxy clusters, underscoring the role of galaxy collisions in the formation of the intergalactic stellar population, since
the frequency of galaxy collisions grows with their density. |
