Star formation by collapse of molecular clouds
Simulation by SPH of the collapse and fragmentation of a molecular cloud presented in The Formation of Stars and Brown Dwarfs and the Truncation of Protoplanetary Discs in a Star Cluster by Matthew R. Bate, Ian A. Bonnell, and Volker Bromm The calculation models the collapse and fragmentation of a molecular cloud with a mass 50 times that of our Sun. The cloud is initially 1. 2 lightyears (9. 5 million million kilometres) in diameter, with a temperature of 10 Kelvin (263 degrees Celsius).
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