The nonisothermal stage of magnetic star formation. II. Results

TL;DR

This paper presents detailed simulations of magnetically-supported star formation, tracking core evolution from initial fragmentation to protostar formation, highlighting the roles of ambipolar diffusion and Ohmic dissipation in magnetic flux decoupling.

Contribution

It provides comprehensive, high-resolution modeling of the entire star formation process, emphasizing the dominant role of ambipolar diffusion over Ohmic dissipation in magnetic decoupling.

Findings

Ambipolar diffusion causes magnetic decoupling at ~3 x 10^12 cm^-3.

Magnetic flux concentrates outside the hydrostatic core, forming a 'magnetic wall'.

The hydrostatic core forms with a radius of about 2 AU and density of 10^14 cm^-3.

Abstract

In a previous paper we formulated the problem of the formation and evolution of fragments (or cores) in magnetically-supported, self-gravitating molecular clouds in axisymmetric geometry, accounting for the effects of ambipolar diffusion and Ohmic dissipation, grain chemistry and dynamics, and radiative transfer. Here we present results of star formation simulations that accurately track the evolution of a protostellar fragment over eleven orders of magnitude in density (from 300 cm^-3 to \approx 10^14 cm^-3), i.e., from the early ambipolar-diffusion--initiated fragmentation phase, through the magnetically supercritical, dynamical-contraction phase and the subsequent magnetic decoupling stage, to the formation of a protostellar core in near hydrostatic equilibrium. As found by Fiedler & Mouschovias (1993), gravitationally-driven ambipolar diffusion leads to the formation and subsequent dynamic contraction of a magnetically supercritical core. Moreover, we find that ambipolar diffusion, not Ohmic dissipation, is responsible for decoupling all the species except the electrons from the magnetic field, by a density \approx 3 x 10^12 cm^-3. Magnetic decoupling precedes the formation of a central stellar object and ultimately gives rise to a concentration of magnetic flux (a `magnetic wall') outside the hydrostatic core --- as also found by Tassis & Mouschovias (2005a,b) through a different approach. At approximately the same density at which Ohmic dissipation becomes more important than ambipolar diffusion (\gtrsim 7 x 10^12 cm^-3), the grains carry most of the electric charge as well as the electric current. The prestellar core remains disclike down to radii ~ 10 AU, inside which thermal pressure becomes important. The magnetic flux problem of star formation is resolved for at least strongly magnetic newborn stars by this stage of the evolution, i.e., by a central density \approx 10^14 cm^-3. The hydrostatic core has radius \approx 2 AU, density \approx 10^14 cm^-3, temperature \approx 300 K, magnetic field strength \approx 0.2 G, magnetic flux \approx 5 x 10^18 Wb, luminosity ~ 10^-3 L_\odot, and mass ~ 10^-2 M_\odot.