Star formation in a galactic cluster

Details Star formation in a galactic cluster Star formation in a galactic cluster

Mar 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979rspta.291..219w&link_type=abstract

Royal Society (London), Philosophical Transactions, Series A, vol. 291, no. 1380, Mar. 27, 1979, p. 219-252.

Physics

16

Galactic Clusters, Gravitational Collapse, Interstellar Matter, Planetary Nebulae, Star Formation, Collision Parameters, Energy Dissipation, Natural Satellites, Planetary Systems, Stellar Mass, Stellar Models, Stellar Rotation

Scientific paper

A model has been developed for the collapse of an interstellar cloud with turbulence. The differential equations that describe the evolution of the cloud include ionic and dust cooling and also the dissipation of energy due to the collision of turbulent elements moving at supersonic speeds. Under some conditions the collision of two elements can give rise to a star, and the rate of star formation and the mass of the stars formed changes as the cloud collapses. The pattern found is that the stars first produced have masses of about 1.4 solar masses and the masses get less as star formation continues. Stars produced by this mechanism have little associated angular momentum. Some of the stars that happen to move in high-density regions of the cloud may increase their mass greatly by accretion; these stars will be the more massive stars and they will also rotate most rapidly, a theoretical prediction that agrees with observation. On the basis of the model the proportion of stars that would have planetary systems is estimated. This shows that there should be of the order of 1 million planetary systems per galaxy.

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