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, Marcio
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.accessioned2025-01-20T16:08:44Z
dc.date.available2025-01-20T16:08:44Z
dc.date.issued2024
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.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/202348307
dc.identifier.eissn1432-0746
dc.identifier.issn0004-6361
dc.identifier.urihttps://doi.org/10.1051/0004-6361/202348307
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/90102
dc.identifier.wosidWOS:001310276200001
dc.language.isoen
dc.revistaAstronomy & astrophysics
dc.rightsacceso restringido
dc.subjectaccretion
dc.subjectaccretion disks
dc.subjectnovae
dc.subjectcataclysmic 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
dc.volumen689
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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