A prescription for the turbulent heating of astrophysical plasmas
Gregory G. Howes
TL;DR
This paper develops a model to predict how turbulence dissipates energy into ions and electrons in astrophysical plasmas, with applications to accretion disks and the interstellar medium.
Contribution
It introduces a new cascade-based model for ion-electron heating ratios in weakly collisional plasmas, expanding understanding of turbulent heating processes.
Findings
Provides a prescription for turbulent heating in astrophysical plasmas.
Predicts ion-electron heating ratios in accretion disks.
Applies the model to interstellar medium conditions.
Abstract
The ratio of ion to electron heating due to the dissipation of Alfvenic turbulence in astrophysical plasmas is calculated based on a cascade model for turbulence in weakly collisional plasmas. Conditions for validity of this model are discussed, a prescription for the turbulent heating is presented, and it is applied to predict turbulent heating in accretion disks and the interstellar medium.
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