Evolution of a Super-Massive Star in a Dense Stellar System

Details Evolution of a Super-Massive Star in a Dense Stellar System Evolution of a Super-Massive Star in a Dense Stellar System

Sep 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978pthph..60..711h&link_type=abstract

Progress of Theoretical Physics, Vol. 60, No. 3, pp. 711-723

Physics

15

Scientific paper

The evolution of a Super-Massive Star (SMS) in a dense stellar system is investigated. As the SMS contracts, the dissipation of the stellar kinetic energy via drag force in the SMS increases and becomes greater than the critical luminosity Lcr of the SMS. Then, the SMS does not contract further. In this stage, the SMS adjusts itself automatically to maintain its luminosity close to the Eddington limit Lcr by expansion or contraction. Through this control, rather regular luminosity variations can be expected in the order of several months. On the other hand, the collisions among the stars in the stellar system contribute to the sudden luminosity variations by about one collision per year or so. The stars trapped in the SMS sink rapidly toward the center of the SMS and form a high density stellar system where most stars may disintegrate into gas by frequent collisions among themselves and form a small SMS of mass ˜ 106m&sun; within the large SMS of mass ˜ 108m&sun;.

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