Nova MON 1942.

Gaposchkin, Sergei

doi:10.1086/106996

Cited by 3 publications

(15 citation statements)

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“…Send offprint requests to: T. Kato, e-mail: tkato@kusastro.kyoto-u.ac.jp Gaposchkin (1954) place it unequivocally as a nova" and suggested that "further study might find KT Mon to be recurrent" based on this unusual distance estimate. Similar long-distance estimates have been given in Warner (1987);Shafter (1997).…”

Section: Introductionmentioning

confidence: 99%

“…The object was first recorded at m pg = 10.3 on 1942 December 30. Gaposchkin (1954) presented a light curve and a description of a spectrum taken by Vyssotsky on the discovery plate. According to Gaposchkin (1954), the object rather rapidly faded (2 mag in 27 d).…”

Section: Introductionmentioning

confidence: 99%

“…Gaposchkin (1954) presented a light curve and a description of a spectrum taken by Vyssotsky on the discovery plate. According to Gaposchkin (1954), the object rather rapidly faded (2 mag in 27 d). The object was fainter than m pg = 13.35, 13.9 d prior to the first positive record on 1942 December 30.…”

Section: Introductionmentioning

confidence: 99%

“…The object was fainter than m pg = 13.35, 13.9 d prior to the first positive record on 1942 December 30. Gaposchkin (1954) described the low-resolution spectrum by Vyssotsky as "broad bright lines Hβ, Hγ, Hδ, 4686 HeII and 4640 NIII". From these findings, Gaposchkin (1954) concluded that KT Mon is a nova.…”

Section: Introductionmentioning

confidence: 99%

“…Gaposchkin (1954) described the low-resolution spectrum by Vyssotsky as "broad bright lines Hβ, Hγ, Hδ, 4686 HeII and 4640 NIII". From these findings, Gaposchkin (1954) concluded that KT Mon is a nova. Duerbeck (1987) classified the object as an established moderately fast nova.…”

Section: Introductionmentioning

confidence: 99%

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Is KT Mon a classical nova?

Katô

Yamaoka

2002

A&A

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Abstract. 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.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Is KT Mon a classical nova?

Katô

Yamaoka

2002

A&A

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Past and Future Novae

Payne-Gaposchkin¹

1977

Novae and Related Stars

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Eclipsing Binary Systems XZ Per and BO Vul with Complex Variations in Orbital Periods

Khaliullina

2021

Astron. Rep.

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The variations in the orbital periods of the eclipsing binary systems XZ Per and BO Vul have been studied. It has been shown that the variations in the orbital period of the eclipsing binary XZ Per are equally well represented as a superposition of the secular decrease and cyclic variations or as a sum of two cyclic variations. In the first case, the monotonic component can be a consequence of the loss of angular momentum by the system due to magnetic braking, while cyclic variations can be explained by the presence of a third body in the system or by the magnetic activity of the secondary component with a convective shell. In the second case, it is possible to assume the presence of two additional bodies in the system, or to attribute one of the period oscillations to the light-time effect, and the other to the magnetic activity of the secondary component. The variations in the orbital period of the eclipsing binary system BO Vul can be represented as a superposition of the secular decrease and cyclic variations. The observed cyclic variations in the period can occur due to the presence of a third body in the system or due to the magnetic activity of the secondary component with a convective shell.

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Nova MON 1942.

Cited by 3 publications

References 0 publications

Is KT Mon a classical nova?

Is KT Mon a classical nova?

Past and Future Novae

Eclipsing Binary Systems XZ Per and BO Vul with Complex Variations in Orbital Periods

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