Reconnection-driven oscillations in dwarf nova disks

Details Reconnection-driven oscillations in dwarf nova disks Reconnection-driven oscillations in dwarf nova disks

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...320..741t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 320, Sept. 15, 1987, p. 741-745. NSF-NASA-supported research.

Astronomy and Astrophysics

Astrophysics

11

Accretion Disks, Dwarf Novae, Magnetic Field Reconnection, Stellar Oscillations, High Reynolds Number, Loci, Magnetic Field Configurations, Magnetohydrodynamics

Scientific paper

A class of oscillations observed during eruption of dwarf novae has been interpreted as oscillations of the accretion disks in these systems. These oscillations are quasi-periodic with coherence times typically between three and 15 cycles. The authors show that magnetic field reconnection at high magnetic Reynolds number (Rm > 106) can drive disk oscillations. The expected stochastic geometry of disk magnetic fields could naturally produce the observed phase incoherency.

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