dc.contributor.author |
Sklyanov A. |
|
dc.contributor.author |
Pavlenko E. |
|
dc.contributor.author |
Antonyuk O. |
|
dc.contributor.author |
Antonyuk K. |
|
dc.contributor.author |
Sosnovsky A. |
|
dc.contributor.author |
Galeev A. |
|
dc.contributor.author |
Pit’ N. |
|
dc.contributor.author |
Babina Y. |
|
dc.date.accessioned |
2018-09-19T21:56:33Z |
|
dc.date.available |
2018-09-19T21:56:33Z |
|
dc.date.issued |
2016 |
|
dc.identifier.issn |
1990-3413 |
|
dc.identifier.uri |
https://dspace.kpfu.ru/xmlui/handle/net/144513 |
|
dc.description.abstract |
© 2016, Pleiades Publishing, Ltd.We report the results of observations of a WZ Sge-type dwarf nova ASASSN-14cv, acquired in 2014 and covering the end of a superoutburst and a rebrightening stage. We detected 8 rebrightenings of this star. Based on the light curve profiles of the rebrightenings, we conclude on the existence of both the “inside-out” and “outside-in” outbursts. During the entire course of the rebrightening stage, a brightness variability with the mean period of P = 0.d06042(8) was detected, which was identified as a superhump period during the stage B of the superoutburst. The character of the registered superhump evolution can be either described by a parabolic approximation with the negative Pdot = −1.1 × 10−5, or by an approximation with 2 linear areas with the corresponding periods of 0.d06074(3) and 0.d06046(9). |
|
dc.relation.ispartofseries |
Astrophysical Bulletin |
|
dc.subject |
accretion: accretion disks |
|
dc.subject |
stars: cataclysmic variables |
|
dc.subject |
stars: dwarf novae |
|
dc.subject |
stars: individual ASASSN-14cv |
|
dc.title |
Superhump evolution of WZ Sge-type dwarf nova ASASSN-14cv at rebrightening stage |
|
dc.type |
Article |
|
dc.relation.ispartofseries-issue |
3 |
|
dc.relation.ispartofseries-volume |
71 |
|
dc.collection |
Публикации сотрудников КФУ |
|
dc.relation.startpage |
293 |
|
dc.source.id |
SCOPUS19903413-2016-71-3-SID84983316552 |
|