### Accretion-driven core collapse and the collisional formation of massive starsAccretion-driven core collapse and the collisional formation of massive stars

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 Author Bonnell, C. Clarke I. Source arXiv.org Content type Text File Format PDF Date of Submission 2008-05-08 Language English
 Subject Domain (in DDC) Computer science, information & general works ♦ Natural sciences & mathematics ♦ Astronomy & allied sciences ♦ Physics Subject Keyword Astrophysics ♦ physics:astro-ph 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. Description Comment: MNRAS accepted Educational Use Research Learning Resource Type Article