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Constraining the Physics of AM Canum Venaticorum Systems with the Accretion Disk Instability ModelRecent work by Levitan et al. has expanded the long-term photometric database for AM CVn stars. In particular, their outburst properties are well correlated with orbital period and allow constraints to be placed on the secular mass transfer rate between secondary and primary if one adopts the disk instability model for the outbursts. We use the observed range of outbursting behavior for AM CVn systems as a function of orbital period to place a constraint on mass transfer rate versus orbital period. We infer a rate approximately 5 x 10(exp -9) solar mass yr(exp -1) ((P(sub orb)/1000 s)(exp -5.2)). We show that the functional form so obtained is consistent with the recurrence time-orbital period relation found by Levitan et al. using a simple theory for the recurrence time. Also, we predict that their steep dependence of outburst duration on orbital period will flatten considerably once the longer orbital period systems have more complete observations.
Document ID
20160011360
Document Type
Reprint (Version printed in journal)
Authors
Cannizzo, John K. (Maryland Univ. Baltimore County Baltimore, MD, United States)
Nelemans, Gijs (Radboud Univ. Nijmegen, Netherlands)
Date Acquired
September 19, 2016
Publication Date
April 9, 2015
Publication Information
Publication: The Astrophysical Journal
Volume: 803
Issue: 1
Subject Category
Astrophysics
Report/Patent Number
GSFC-E-DAA-TN34675
Funding Number(s)
CONTRACT_GRANT: NNG06EO90A
Distribution Limits
Public
Copyright
Other
Keywords
accretion
accretion disks
aEuro" binaries: close aEuro" novae