On the origin of episodic accretion in Dwarf Novae

Preprint

23 October 1997

preprint
Published by arXiv in arXiv

https://doi.org/10.48550/arXiv.astro-ph/9710250

Abstract

We show that dwarf nova disks in quiescence have rather low magnetic Reynolds number, of order 10^3. Numerical simulations of magnetized accretion disks suggest that under these conditions magnetohydrodynamic turbulence and the associated angular momentum transport is sharply reduced. This could be the physical origin of episodic accretion in dwarf nova disks. If so, the standard disk instability model needs to be revised.

Keywords

NUMERICAL SIMULATIONS
ORIGIN OF EPISODIC
ACCRETION IN DWARF
EPISODIC ACCRETION
ANGULAR MOMENTUM
REYNOLDS NUMBER
DWARF NOVA
TURBULENCE

All Related Versions

Version 1, 1997-10-23, ArXiv
Published version: The Astrophysical Journal, 492 (1), L75.

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