Ambipolar Drift Heating in Turbulent Molecular Clouds

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© 2000. The American Astronomical Society. All rights reserved. Printed in U.S.A.
, , Citation Paolo Padoan et al 2000 ApJ 540 332 DOI 10.1086/309299

This article is corrected by 2012 ApJ 755 182

0004-637X/540/1/332

Abstract

We present calculations of frictional heating by ion-neutral drift in three-dimensional simulations of turbulent, magnetized molecular clouds. We show that ambipolar drift heating is a strong function of position in a turbulent cloud, and its average value can be significantly larger than the average cosmic-ray heating rate. The heating rate per unit volume due to ambipolar drift, HAD = | ×|2iνin ~ B4/(16π2Lρiνin), is found to depend on the rms Alfvénic Mach number, Script MA, and on the average field strength, as HADScript M⟨|B|⟩4. This implies that the typical scale of variation of the magnetic field, LB, is inversely proportional to Script MA, which we also demonstrate.

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10.1086/309299