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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 |