Volume 396, Number 2, December III 2002
|Page(s)||629 - 632|
|Section||Interstellar and circumstellar matter|
|Published online||03 December 2002|
Is KT Mon a classical nova?
Department of Astronomy, Kyoto University, Kyoto 606-8502, Japan
2 Faculty of Science, Kyushu University, Fukuoka 810-8560, Japan
Corresponding author: T. Kato, firstname.lastname@example.org
Accepted: 15 October 2002
KT Mon has been considered as a classical nova in 1942 based on its light curve and spectroscopy. However, we noticed a unusual feature for a nova soon after its maximum: the early presence of high excitation emission lines such as HeII and NIII. We propose previously overlooked interpretations that KT Mon can be either a WZ Sge-type dwarf nova and an X-ray transient, although the possibility of an unusual or a recurrent nova is not completely excluded. If KT Mon is a WZ Sge-type dwarf nova, the system is expected to have a brown dwarf secondary. If KT Mon is an X-ray transient, the system is a good candidate for the nearest black-hole binary. Within our knowledge, the observed features seem to more strongly support the latter possibility. In all possibilities, we can expect a recurrent outburst in meaningfully near future.
Key words: accretion, accretion disks / novae, cataclysmic variables / stars: dwarf novae / X-rays: bursts / stars: individual: KT Mon
© ESO, 2002
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