Unveiling the nature of two dwarf novae: CRTS J080846.2+313106 and V416 Dra

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dc.contributor.authorJoshi, Arti
dc.contributor.authorCatelan, Márcio
dc.contributor.authorScaringi, Simone
dc.contributor.authorSchwope, Axel
dc.contributor.authorAnupama G.C.
dc.contributor.authorRawat, Nikita
dc.contributor.authorSahu, Devendra K.
dc.contributor.authorSingh, Mridweeka
dc.contributor.authorDastidar, Raya
dc.contributor.authorSubramanian, Rama Venkata
dc.contributor.authorRao, Srinivas M.
dc.date.accessioned2024-10-15T17:23:56Z
dc.date.available2024-10-15T17:23:56Z
dc.date.issued2024-09-01
dc.descriptionIndexación: Scopus.
dc.description.abstractWe present the analysis of optical photometric and spectroscopic observations of two non-magnetic cataclysmic variables, namely CRTS J080846.2+313106 and V416 Dra. We find CRTS J080846.2+313106 to vary with a period of 4.9116 ± 0.0003 h, which was not found in earlier studies and which we provisionally suggest is the orbital period of the system. In both long-period systems, the observed dominant signal at the second harmonic of the orbital frequency and the orbital modulation during quiescence are suggestive of ellipsoidal variation from changing aspects of the secondary, with an additional contribution from the accretion stream or hotspot. However, during the outburst, the hotspot itself is overwhelmed by the increased brightness, which is possibly associated with the accretion disc. The mid-eclipse phase for V416 Dra occurs earlier and the width of the eclipse is greater during outbursts compared to quiescence, suggesting an increased accretion disc radius during outbursts. Furthermore, from our investigation of the accretion disc eclipse in V416 Dra, we find that a total disc eclipse is possible during quiescence, whereas the disc seems to be partially obscured during outbursts, which further signifies that the disc may grow in size as the outburst progresses. The optical spectra of CRTS J080846.2+313106 and V416 Dra are typical of dwarf novae during quiescence, and they both show a significant contribution from the M2-4V secondary. The light curve patterns, orbital periods, and spectra observed in the two systems look remarkably similar, and seem to resemble the characteristics of U Gem-type dwarf novae.
dc.description.urihttps://www-scopus-com.recursosbiblioteca.unab.cl/record/display.uri?eid=2-s2.0-85203880264&origin=resultslist&sort=plf-f&src=s&sid=50bbf553ea681b60a58860a79423c8a9&sot=aff&sdt=cl&cluster=scofreetoread%2C%22all%22%2Ct&s=AF-ID%2860002636%29+AND+SUBJAREA%28PHYS%29&sl=34&sessionSearchId=50bbf553ea681b60a58860a79423c8a9&relpos=6
dc.identifier.citationAstronomy and Astrophysics Open Access Volume 6891 September 2024 Article number A158
dc.identifier.doi10.1051/0004-6361/202348307
dc.identifier.issn00046361
dc.identifier.urihttps://repositorio.unab.cl/handle/ria/61321
dc.language.isoen
dc.publisherEDP Sciences
dc.rights.licenseAttribution 4.0 International CC BY 4.0 Deed
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.subjectaccretion, accretion disks
dc.subjectnovae, cataclysmic variables
dc.subjectstars: individual: CRTS J080846.2+313106
dc.subjectstars: individual: V416 Dra
dc.titleUnveiling the nature of two dwarf novae: CRTS J080846.2+313106 and V416 Dra
dc.typeArtículo
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