On the Photometric Properties of Superhumps in Dwarf Novae of the SU UMa Type

Details On the Photometric Properties of Superhumps in Dwarf Novae of the SU UMa Type On the Photometric Properties of Superhumps in Dwarf Novae of the SU UMa Type

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aca....55..367s&link_type=abstract

Acta Astronomica, v.55, pp.367-374, (2005).

Astronomy and Astrophysics

Astronomy

2

Accretion, Accretion Disks, Novae, Cataclysmic Variables, Stars: Dvarf Novae

Scientific paper

It is shown that in order to account for the observed superhump amplitudes: A_V approx 0.3 mag near superoutburst maximum and A_V approx 0.2 mag at mid-outburst, the temperature of the superhump source must be - respectively - T_sh approx 25000-30000 K and T_sh approx 15000-20000 K.
The resulting bolometric amplitudes of the superhump turn out roughly the same as the visual amplitudes. Accordingly, the excess bolometric luminosity contributed by the superhump source is L_sh approx 3 times 10^34 erg/s near superoutburst maximum, and approx 4 times 10^33 erg/s at mid-outburst. This imposes severe constraints on superhump models.

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