Fast methods to track grain coagulation and ionization. II. Extension to thermal ionization

Abstract

Thermal ionization is a critical process at temperatures T > 10 3 K, particularly during star formation. An increase in ionization leads to a decrease in nonideal magnetohydrodynamics (MHD) resistivities, which has a significant impact on protoplanetary disks and protostar formation. We developed an extension of the fast computational ionization method presented in our recent paper to include thermal ionization. The model can be used to inexpensively calculate the density of ions and electrons and the electric charge of each size of grains for an arbitrary size distribution. This tool should be particularly useful for the self-consistent calculation of nonideal MHD resistivities in multidimensional simulations, especially of protostellar collapse and protoplanetary disks.

Accepted in A&A. 7 pages, 6 figures

References in corpus (5)

• Mineral Processing by Short Circuits in Protoplanetary Disks
• X-ray Super-Flares From Pre-Main Sequence Stars: Flare Energetics And Frequency
• Dependence of Hall Coefficient on Grain Size and Cosmic Ray Rate and Implication for Circumstellar Disk Formation
• Fast methods for tracking grain coagulation and ionization. I. Analytic derivation
• Temperature Fluctuations driven by Magnetorotational Instability in Protoplanetary Disks

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