Superhumps and Accretion Disk Precession in TT ARIETIS

Details Superhumps and Accretion Disk Precession in TT ARIETIS Superhumps and Accretion Disk Precession in TT ARIETIS

Aug 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...503l..67s&link_type=abstract

Astrophysical Journal Letters v.503, p.L67

Astronomy and Astrophysics

Astronomy

35

Accretion, Accretion Disks, Stars: Novae, Cataclysmic Variables, Stars: Individual Constellation Name: Tt Arietis

Scientific paper

We have been conducting a long-term (1988-1998) photometric study of the nova-like variable TT Arietis. The main periodic signal in the star's light curve normally occurs at a period that varies but averages ~0.1329 days, which is about 3.5% shorter than the orbital period of the binary. In 1997, this signal disappeared and was replaced by a stronger signal 8.5% longer than the orbital period. This new wave strongly resembles the"superhumps" commonly seen in SU UMa-type dwarf novae during superoutburst. In superhump parlance, we could say that a negative superhump was replaced by a positive superhump ( P>P_{{orb}} ). This could signify the development of an eccentric instability in the accretion disk. The two superhumps probably signify two types of disk precession: apsidal advance and nodal regression. TT Ari is an excellent candidate for observational studies that probe the origin of superhumps.

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