| Form of presentation | Articles in international journals and collections |
| Year of publication | 2021 |
| Язык | английский |
|
Shimanskiy Vladislav Vladimirovich, author
|
| Bibliographic description in the original language |
Pavlenko E, Kato T, Antonyuk K, MASTER OT J172758.09+380021.5: a peculiar ER UMa-type dwarf nova, probably a missed nova in the recent past//Contributions of the Astronomical Observatory Skalnate Pleso. - 2021. - Vol.51, Is.2. - P.138-162. |
| Annotation |
A CCD photometry of the dwarf nova MASTER OT J172758.09+380021.5 was carried out in 2019 during 134 nights. Observations covered three superoutbursts, ve normal outbursts and quiescence between them. The available ASASSN and ZTF data for 2014 { 2020 were also examined. Spectral observations were done in 2020 when the object was in quiescence. Spectra and photometry revealed that the star is an H-rich active ER UMa-type dwarf nova with a highly variable supercycle (time interval between two successive superoutbursts) of 50 { 100 d that implies a high and variable mass-transfer rate. MASTER OT J172758.09+380021.5 demonstrated peculiar behaviour: short-lasted superoutbursts (a week); a slow superoutburst decline and cases of rebrightenings; low frequency (from none to a few) of the normal outbursts during the supercycle. In 2019 a mean period of positive superhumps was found to be 0.05829 d during the superoutbursts. Late superhumps with a mean period of 0.057915 d which lasted about 20 d after the end of superoutburst and were replaced by an orbital period of 0.057026 d or its orbital-negative superhump beat period were detected. An absence of eclipse in the orbital light curve and its moderate amplitude are consistent with the orbital inclination of about 40 found from spectroscopy. The blue peaks of the V-Ic and B-Rc colour indices of superhumps during the superoutburst coincided with minima of the light curves, while B-Rc of the late superhumps coincided with a rising branch of the light curves. We found that a low mass ratio q = 0:08 could explain most of the peculiarities of MASTER OT J172758.09+380021.5. The mass-transfer rate should be accordingly higher than what is expected from gravitational radiation only, this assumes the object is in a post-nova state and underwent a nova eruption relatively recently { hundreds of years ago. This object would provide probably the rst observational evidence that a nova eruption can occur even in CVs near the period minimum. Key words: stars: MASTER OT J172758.09+380021.5 |
| Keywords |
stars: MASTER OT J172758.09+380021.5 { dwarf novae { ac-
tivity |
| The name of the journal |
Contributions of the Astronomical Observatory Skalnate Pleso
|
| URL |
https://www.scopus.com/inward/record.uri?eid=2-s2.0-85104743382&doi=10.31577%2fcaosp.2021.51.2.138&partnerID=40&md5=711ceafa6b275c063b457a705a40e783 |
| Please use this ID to quote from or refer to the card |
https://repository.kpfu.ru/eng/?p_id=254965&p_lang=2 |
Full metadata record  |
| Field DC |
Value |
Language |
| dc.contributor.author |
Shimanskiy Vladislav Vladimirovich |
ru_RU |
| dc.date.accessioned |
2021-01-01T00:00:00Z |
ru_RU |
| dc.date.available |
2021-01-01T00:00:00Z |
ru_RU |
| dc.date.issued |
2021 |
ru_RU |
| dc.identifier.citation |
Pavlenko E, Kato T, Antonyuk K, MASTER OT J172758.09+380021.5: a peculiar ER UMa-type dwarf nova, probably a missed nova in the recent past//Contributions of the Astronomical Observatory Skalnate Pleso. - 2021. - Vol.51, Is.2. - P.138-162. |
ru_RU |
| dc.identifier.uri |
https://repository.kpfu.ru/eng/?p_id=254965&p_lang=2 |
ru_RU |
| dc.description.abstract |
Contributions of the Astronomical Observatory Skalnate Pleso |
ru_RU |
| dc.description.abstract |
A CCD photometry of the dwarf nova MASTER OT J172758.09+380021.5 was carried out in 2019 during 134 nights. Observations covered three superoutbursts, ve normal outbursts and quiescence between them. The available ASASSN and ZTF data for 2014 { 2020 were also examined. Spectral observations were done in 2020 when the object was in quiescence. Spectra and photometry revealed that the star is an H-rich active ER UMa-type dwarf nova with a highly variable supercycle (time interval between two successive superoutbursts) of 50 { 100 d that implies a high and variable mass-transfer rate. MASTER OT J172758.09+380021.5 demonstrated peculiar behaviour: short-lasted superoutbursts (a week); a slow superoutburst decline and cases of rebrightenings; low frequency (from none to a few) of the normal outbursts during the supercycle. In 2019 a mean period of positive superhumps was found to be 0.05829 d during the superoutbursts. Late superhumps with a mean period of 0.057915 d which lasted about 20 d after the end of superoutburst and were replaced by an orbital period of 0.057026 d or its orbital-negative superhump beat period were detected. An absence of eclipse in the orbital light curve and its moderate amplitude are consistent with the orbital inclination of about 40 found from spectroscopy. The blue peaks of the V-Ic and B-Rc colour indices of superhumps during the superoutburst coincided with minima of the light curves, while B-Rc of the late superhumps coincided with a rising branch of the light curves. We found that a low mass ratio q = 0:08 could explain most of the peculiarities of MASTER OT J172758.09+380021.5. The mass-transfer rate should be accordingly higher than what is expected from gravitational radiation only, this assumes the object is in a post-nova state and underwent a nova eruption relatively recently { hundreds of years ago. This object would provide probably the rst observational evidence that a nova eruption can occur even in CVs near the period minimum. Key words: stars: MASTER OT J172758.09+380021.5 |
ru_RU |
| dc.language.iso |
ru |
ru_RU |
| dc.subject |
|
ru_RU |
| dc.title |
MASTER OT J172758.09+380021.5: a peculiar ER UMa-type dwarf nova, probably a missed nova in the recent past |
ru_RU |
| dc.type |
Articles in international journals and collections |
ru_RU |
|
RUS 
中文 
ES 
Sitemap
