Theory of Collapse and Protostar Formation

Boss, A. P.

doi:10.1007/978-94-009-3861-8_14

A. P. Boss³

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 134))

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Abstract

Interstellar clouds must increase in density by a factor of more than 10²⁰ in order to form stars. Because observations of the phases intermediate between dense interstellar clouds and pre-main-sequence stars are difficult, theoretical solutions presently provide the primary means for exploring the collapse phase of protostellar formation. The mathematical formulation of the protostellar collapse problem is presented, and various methods employed in solving the equations are outlined. This tutorial emphasizes the numerical approach to the study of the nonlinear, time dependent evolution of collapsing interstellar clouds, including self-gravit at ion, rotation, and radiative transfer. Results are summarized for the restricted cases of spherical and axisymmetric symmetry, as well as for fully three dimensional evolutions, and briefly compared to observations of star formation.

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DTM, Carnegie Institution of Washington, 5241 Broad Branch Road, N.W, Washington, DC, 20015, USA
A. P. Boss

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NASA Ames Research Center, Moffett Field, California, USA
David J. Hollenbach
Department of Physics and Astronomy, The University of Wyoming, Laramie, Wyoming, USA
Harley A. Thronson Jr.

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Boss, A.P. (1987). Theory of Collapse and Protostar Formation. In: Hollenbach, D.J., Thronson, H.A. (eds) Interstellar Processes. Astrophysics and Space Science Library, vol 134. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3861-8_14

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DOI: https://doi.org/10.1007/978-94-009-3861-8_14
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