An empirical model for protostellar collapse

Abstract

We propose a new analytic model for the initial conditions of protostellar collapse in relatively isolated regions of star formation. The model is non-magnetic, and is based on a Plummer-like radial density profile as its initial condition. It fits: the observed density profiles of pre-stellar cores and Class 0 protostars; recent observations in pre-stellar cores of roughly constant contraction velocities over a wide range of radii; and the lifetimes and accretion rates derived for Class 0 and Class I protostars. However, the model is very simple, having in effect only 2 free parameters, and so should provide a useful framework for interpreting observations of pre-stellar cores and protostars, and for calculations of radiation transport and time-dependent chemistry. As an example, we model the pre-stellar core L1544.

To appear in Astrophysical Journal, Jan 20th, 2001. 18 pages incl. 3 figs

References in corpus (2)

• First Observations of the Magnetic Field Geometry in Pre-stellar Cores
• How to Identify Pre-Protostellar Cores

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