On the Origin of Episodic Accretion in Dwarf Novae
Open Access
- 1 January 1998
- journal article
- research article
- Published by American Astronomical Society in The Astrophysical Journal
- Vol. 492 (1) , L75-L78
- https://doi.org/10.1086/311091
Abstract
We show that dwarf nova disks in quiescence have rather low magnetic Reynolds numbers, of order 103. 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
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This publication has 25 references indexed in Scilit:
- X‐Ray Ionization of Protoplanetary DisksThe Astrophysical Journal, 1997
- Nonlinear Stability, Hydrodynamical Turbulence, and Transport in DisksThe Astrophysical Journal, 1996
- Numerical Simulations of Circumstellar Disk ConvectionThe Astrophysical Journal, 1996
- Layered Accretion in T Tauri DisksThe Astrophysical Journal, 1996
- Dynamo-driven Accretion Disks and Dwarf Nova EruptionsThe Astrophysical Journal, 1996
- Dynamo-generated Turbulence and Large-Scale Magnetic Fields in a Keplerian Shear FlowThe Astrophysical Journal, 1995
- THE LIMIT CYCLE INSTABILITY IN DWARF NOVA ACCRETION DISKSThe Chaotic Universe, 1993
- The Accretion Disk Limit Cycle Model: Toward an Understanding of the Long-Term Behavior of SS CygniThe Astrophysical Journal, 1993
- A powerful local shear instability in weakly magnetized disks. I - Linear analysis. II - Nonlinear evolutionThe Astrophysical Journal, 1991
- On the spontaneous magnetic field in a conducting liquid in turbulent motionProceedings of the Royal Society of London. Series A. Mathematical and Physical Sciences, 1950