Classical Novae Masquerading as Dwarf Novae? Outburst Properties of Cataclysmic Variables with ASAS-SN

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dc.contributor.authorKawash, Adam
dc.contributor.authorChomiuk, Laura
dc.contributor.authorStrader, Jay
dc.contributor.authorAydi, Elias
dc.contributor.authorSokolovsky, Kirill V.
dc.contributor.authorJayasinghe, Tharindu
dc.contributor.authorKochanek, Chris S.
dc.contributor.authorSchmeer, Patrick
dc.contributor.authorStanek, Krzysztof Z.
dc.contributor.authorMukai, Koji
dc.contributor.authorShappee, Ben
dc.contributor.authorWay, Zachary
dc.contributor.authorBasinger, Connor
dc.contributor.authorHoloien, Tom W.-S.
dc.contributor.authorPrieto, Jose L.
dc.date.accessioned2021-03-12T19:24:07Z
dc.date.available2021-03-12T19:24:07Z
dc.date.issued2021-01-28
dc.description.abstractThe unprecedented sky coverage and observing cadence of the All-Sky Automated Survey for SuperNovae (ASAS-SN) has resulted in the discovery and continued monitoring of a large sample of Galactic transients. The vast majority of these are accretion-powered dwarf nova outbursts in cataclysmic variable systems, but a small subset are thermonuclear-powered classical novae. Despite improved monitoring of the Galaxy for novae from ASAS-SN and other surveys, the observed Galactic nova rate is still lower than predictions. One way classical novae could be missed is if they are confused with the much larger population of dwarf novae. Here, we examine the properties of 1617 dwarf nova outbursts detected by ASAS-SN and compare them to classical novae. We find that the mean classical nova brightens by ~11 magnitudes during outburst, while the mean dwarf nova brightens by only ~5 magnitudes, with the outburst amplitude distributions overlapping by roughly 15%. For the first time, we show that the amplitude of an outburst and the time it takes to decline by two magnitudes from maximum are positively correlated for dwarf nova outbursts. For classical novae, we find that these quantities are negatively correlated, but only weakly, compared to the strong anti-correlation of these quantities found in some previous work. We show that, even if located at large distances, only a small number of putative dwarf novae could be mis-classified classical novae suggesting that there is minimal confusion between these populations. Future spectroscopic follow-up of these candidates can show whether any are indeed classical novae.en_US
dc.description.sponsorshipThis research has made use of the International Variable Star Index (VSX) database, operated at AAVSO, Cambridge, Massachusetts, USA. We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. A.K., L.C., E.A., and K.V.S. acknowledge financial support of NSF award AST-1751874 and a Cottrell fellowship of the Research Corporation. J.S. acknowledges support from the Packard Foundation. BJS, CSK, and KZS are supported by NSF grant AST-1907570. CSK and KZS are supported by NSF grant AST-181440. We thank the Las Cumbres Observatory and its staff for its continuing support of the ASAS-SN project. ASAS-SN is supported by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University, and NSF grants AST-1515927 and AST1908570. Development of ASAS-SN has been supported by NSF grant AST-0908816, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Chinese Academy of Sciences South America Center for Astronomy (CAS- SACA), and the Villum Foundation.en_US
dc.description.urihttps://arxiv.org/abs/2101.12239en_US
dc.format.extent24 pagesen_US
dc.genrejournal articles preprintsen_US
dc.identifierdoi:10.13016/m2qy3h-ire2
dc.identifier.citationKawash, Adam; Chomiuk, Laura; Strader, Jay; Aydi, Elias; Sokolovsky, Kirill V.; Jayasinghe, Tharindu; Kochanek, Chris S.; Schmeer, Patrick; Stanek, Krzysztof Z.; Mukai, Koji; Shappee, Ben; Way, Zachary; Basinger, Connor; Holoien, Tom W.-S.; Prieto, Jose L.; Classical Novae Masquerading as Dwarf Novae? Outburst Properties of Cataclysmic Variables with ASAS-SN; Solar and Stellar Astrophysics (2021); https://arxiv.org/abs/2101.12239en_US
dc.identifier.urihttp://hdl.handle.net/11603/21178
dc.language.isoen_USen_US
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Physics Department Collection
dc.relation.ispartofUMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
dc.relation.ispartofUMBC Faculty Collection
dc.rightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
dc.rightsAttribution 4.0 International (CC BY 4.0)*
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/*
dc.titleClassical Novae Masquerading as Dwarf Novae? Outburst Properties of Cataclysmic Variables with ASAS-SNen_US
dc.typeTexten_US

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