Flaring, Dust Formation, And Shocks In The Very Slow Nova ASASSN-17pf (LMCN 2017-11a)

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dc.contributor.authorAydi, E.
dc.contributor.authorChomiuk, L.
dc.contributor.authorStrader, J.
dc.contributor.authorSwihart, S. J.
dc.contributor.authorBahramian, A.
dc.contributor.authorHarvey, E. J.
dc.contributor.authorBritt, C. T.
dc.contributor.authorBuckley, D. A. H.
dc.contributor.authorChen, P.
dc.contributor.authorDage, K.
dc.contributor.authorDarnley, M. J.
dc.contributor.authorDong, S.
dc.contributor.authorHambsch, F-J.
dc.contributor.authorHoloien, T. W.-S.
dc.contributor.authorJha, S. W.
dc.contributor.authorKochanek, C. S.
dc.contributor.authorKuin, N. P. M.
dc.contributor.authorLi, K. L.
dc.contributor.authorMonard, L. A. G.
dc.contributor.authorMukai, K.
dc.contributor.authorPage, K. L.
dc.contributor.authorPrieto, J. L.
dc.contributor.authorRichardson, N. D.
dc.contributor.authorShappee, B. J.
dc.contributor.authorShishkovsky, L.
dc.contributor.authorSokolovsky, K. V.
dc.contributor.authorStanek, K. Z.
dc.contributor.authorThompson, T.
dc.date.accessioned2019-06-25T17:18:27Z
dc.date.available2019-06-25T17:18:27Z
dc.date.issued2019-03-21
dc.description.abstractWe present a detailed study of the 2017 eruption of the classical nova ASASSN-17pf (LMCN 2017-11a), which is located in the Large Magellanic Cloud, including data from AAVSO, ASAS-SN, SALT, SMARTS, SOAR, and the Neil Gehrels Swift Observatory. The optical light-curve is characterized by multiple maxima (flares) on top of a slowly evolving light-curve (with a decline time, t2> 100 d). The maxima correlate with the appearance of new absorption line systems in the optical spectra characterized by increasing radial velocities. We suggest that this is evidence of multiple episodes of mass-ejection with increasing expansion velocities. The line profiles in the optical spectra indicate very low expansion velocities (FWHM ∼ 190 km s−1), making this nova one of the slowest expanding ever observed, consistent with the slowly evolving light-curve. The evolution of the colors and spectral energy distribution show evidence of decreasing temperatures and increasing effective radii for the pseudo-photosphere during each maximum. The optical and infrared light-curves are consistent with dust formation 125 days post-discovery. We speculate that novae showing several optical maxima have multiple mass-ejection episodes leading to shocks that may drive γ-ray emission and dust formationen_US
dc.description.sponsorshipEA, LC, and KVS acknowledge NSF award AST1751874, NASA award 11-Fermi 80NSSC18K1746, and a Cottrell fellowship of the Research Corporation. JS was supported by the Packard Foundation. MJD acknowledges funding from the UK Science & Technology Facilities Council. KLP and NPMK acknowledge support from the UK Space Agency. PC and SD acknowledge NSFC Project 11573003. TAT acknowledges support from a Simons Foundation Fellowship and from an IBM Einstein Fellowship from the Institute for Advanced Study, Princeton. NDR is grateful for postdoctoral support by the University of Toledo and by the Helen Luedtke Brooks Endowed Professorship. SWJ is supported by NSF award AST-1615455. DAHB gratefully acknowledges the receipt of research grants from the National Research Foundation (NRF) of South Africa. ASAS-SN thanks 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 grant AST1515927. 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 (CASSACA), the Villum Foundation, and George Skestos.en_US
dc.description.urihttps://arxiv.org/abs/1903.09232en_US
dc.format.extent31 pagesen_US
dc.genrejournal articles preprintsen_US
dc.identifierdoi:10.13016/m2gznv-us6b
dc.identifier.citationE. Aydi, et.al, Flaring, Dust Formation, And Shocks In The Very Slow Nova ASASSN-17pf (LMCN 2017-11a), High Energy Astrophysical Phenomena, 2019, https://arxiv.org/abs/1903.09232en_US
dc.identifier.urihttp://hdl.handle.net/11603/14306
dc.language.isoen_USen_US
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Center for Space Sciences and Technology
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.subjectstars: individual (ASASSN-17pf)en_US
dc.subjectnovaeen_US
dc.subjectcataclysmic variablesen_US
dc.subjectwhite dwarfsen_US
dc.titleFlaring, Dust Formation, And Shocks In The Very Slow Nova ASASSN-17pf (LMCN 2017-11a)en_US
dc.typeTexten_US

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