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- W2949269029 abstract "We consider the conditions required for a cluster core to shrink, by adiabatic accretion of gas from the surrounding cluster, to densities such that stellar collisions are a likely outcome. We show that the maximum densities attained, and hence the viability of collisions, depends on a competition between core shrinkage (driven by accretion) and core puffing up (driven by relaxation effects). The expected number of collisions scales as $N_{core}^{5/3} tilde v^2$ where $N_{core}$ is the number of stars in the cluster core and $tilde v$ is the free fall velocity of the parent cluster (gas reservoir). Thus whereas collisions are very unlikely in a relatively low mass, low internal velocity system such as the Orion Nebula Cluster, they become considerably more important at the mass and velocity scale characteristic of globular clusters. Thus stellar collisions in response to accretion induced core shrinkage remains a viable prospect in more massive clusters, and may contribute to the production of intermediate mass black holes in these systems." @default.
- W2949269029 created "2019-06-27" @default.
- W2949269029 creator A5059337593 @default.
- W2949269029 date "2008-05-08" @default.
- W2949269029 modified "2023-09-27" @default.
- W2949269029 title "Accretion-driven core collapse and the collisional formation of massive stars" @default.
- W2949269029 hasPublicationYear "2008" @default.
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