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The 2003 Superoutburst of a New SU UMa-Type Dwarf Nova, GO Comae Berenices

Published online by Cambridge University Press:  22 February 2018

Akira Imada ,
Makoto Uemura ,
Ryoko Ishioka ,
Daisaku Nogami ,
Taichi Kato  and
VSNET Collaboration Team
Akira Imada
Affiliation:
Department of Astronomy, Kyoto University, Kyoto, 606-8502, Japan (a_imada@kusastro.kyoto-u.ac.jp)
Makoto Uemura
Affiliation:
Department of Astronomy, Kyoto University, Kyoto, 606-8502, Japan (a_imada@kusastro.kyoto-u.ac.jp)
Ryoko Ishioka
Affiliation:
Department of Astronomy, Kyoto University, Kyoto, 606-8502, Japan (a_imada@kusastro.kyoto-u.ac.jp)
Daisaku Nogami
Affiliation:
Department of Astronomy, Kyoto University, Kyoto, 606-8502, Japan (a_imada@kusastro.kyoto-u.ac.jp)
Taichi Kato
Affiliation:
Department of Astronomy, Kyoto University, Kyoto, 606-8502, Japan (a_imada@kusastro.kyoto-u.ac.jp)

Extract

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We photometrically observed the 2003 superoutburst of GO Com, which is a candidate for WZ Sge-type dwarf novae (WZ). However, the obtained light curve is atypical of both types: a plateau stage is too short for SU UMa-type dwarf novae (SU) while the amplitude of the superoutburst is too small for WZ. In order to explain this behavior, it might be taken into account that the mass accretion onto the white dwarf is efficient during quiescence.

Type
The Contributed Papers
Information
International Astronomical Union Colloquium , Volume 194: Compact binaries in the galaxy and beyond , 2004 , pp. 265
Copyright
Copyright © Instituto de astronomia/revista mexicana de astronomίa y astrofίsica 2004

References

Kato, T. 1997, PASJ, 49, 583 Google Scholar