Evolution of rotating interstellar clouds. II - The collapse of protostars of 1, 2, and 5 solar masses

Details Evolution of rotating interstellar clouds. II - The collapse of protostars of 1, 2, and 5 solar masses Evolution of rotating interstellar clouds. II - The collapse of protostars of 1, 2, and 5 solar masses

May 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...206..138b&link_type=abstract

Astrophysical Journal, vol. 206, May 15, 1976, pt. 1, p. 138-149.

Astronomy and Astrophysics

Astrophysics

88

Gravitational Collapse, Interstellar Matter, Protostars, Rotating Matter, Stellar Evolution, Angular Momentum, Density Distribution, Hydrodynamics, Jeans Theory, Ring Structures

Scientific paper

Numerical calculations have been made for the early stages of collapse of axisymmetric rotating protostars of 1, 2, and 5 solar masses. The calculations employ a range of values of total angular momentum, as well as two types of initial density distribution. The effects of boundary conditions are tested by using constant volume and constant surface pressure with identical initial conditions. The principal result of the calculations is that, in all cases tried, the collapse leads to the formation of a ring structure in the interior of the cloud, with a local density minimum at the center of the cloud. The rings approach equilibrium with a structure consistent with that of previous analytic determinations, after which they undergo further gravitational collapse. The collapse of a two-solar-mass cloud, similar to that assumed by Cameron and Pine (1973), does not appear to lead to the equilibrium nebula these authors construct.

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