On the nature of dwarf novae

Details On the nature of dwarf novae On the nature of dwarf novae

Sep 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...272..234s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 272, Sept. 1, 1983, p. 234-237.

Astronomy and Astrophysics

Astrophysics

56

Binary Stars, Dwarf Novae, Mass Transfer, Mass Ratios, Radii, Rates (Per Time), Stellar Mass Accretion

Scientific paper

Observational data on mass transfer rates and radii of disks indicate that the outer parts of disks in novae and nova-like binaries are sufficiently hot for stationary accretion; those in dwarf novae are too cool to avoid an accretion instability; while those in Z Cam systems are the borderline cases. The mass ratios of novae and nova-like binaries with main-sequence secondaries appear - at a given orbital period - to be systematically larger than those of dwarf novae, implying that higher mass ratios are responsible for higher mass transfer rates.

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