Superhumps, resonances and accretion discs

Details Superhumps, resonances and accretion discs Superhumps, resonances and accretion discs

Mar 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.249...25w&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 249, March 1, 1991, p. 25-35.

Astronomy and Astrophysics

Astronomy

183

Accretion Disks, Dwarf Novae, Orbital Resonances (Celestial Mechanics), Gas Dynamics, Stellar Evolution, Stellar Mass Accretion, Stellar Orbits

Scientific paper

The structure of accretion disks within binary systems is shown to be influenced by the excitation of resonances within the disk. Of particular importance is the near 3:1 commensurability with the stars' orbit. This can be used to explain the superhump phenomenon of SU Ursae Majoris dwarf novae in superoutburst. This resonance can only appear for mass ratios which satisfy M2/M1 less than about 0.25-0.33; for larger mass ratios, the available resonances are weaker and of the wrong form to produce the superhump phenomenon. The mass-transfer stream is shown to be an important contributor to the growth rate of the resonance.

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