Abstract
The ER UMa-type, including ER UMa, VI159 Ori and RZ LMi, is a subgroup of SU UMa-type dwarf novae. Outbursts of these stars are characterized by: (i) the extremely short recurrence time of the superoutburst (∼ 40 d in ER UMa and V1159 Ori, ∼ 20 d in RZ LMi), (ii) short outbursts with short recurrence times (∼ 4 d) between the bright states, and (iii) extremely long duty cycles (∼ 0.5). Assuming that the mass transfer rate from the secondary is ten times higher than that of ordinary SU UMa stars, which was invoked by Kato & Kunjaya (1995), and a weak tidal torque in the case of RZ LMi, Osaki (1996) showed that the light curves of these stars can be reproduced by the disk instability model, which does not require mass transfer bursts. These indicate that ER UMa, VI159 Ori and RZ LMi are not on the natural extension of SU UMa-type dwarf novae.
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References
Kato, T., Kunjaya, C, 1995, PASJ, 47, 163
Osaki, Y., 1996, these proceedings, pl27
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© 1996 Kluwer Academic Publishers
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Nogami, D. et al. (1996). New Observational Frontiers of Er Uma (= PG 0943+521) Type Dwarf Novae. In: Evans, A., Wood, J.H. (eds) Cataclysmic Variables and Related Objects. Astrophysics and Space Science Library, vol 208. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0325-8_16
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DOI: https://doi.org/10.1007/978-94-009-0325-8_16
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