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Title: Swift detection of the super-swift switch-on of the super-soft phase in nova V745 Sco (2014)
Authors: Page, Kim L.
Osborne, Julian Paul
Kuin, N. P. M.
Henze, M.
Walter, F. M.
Beardmore, Andrew P.
Bode, M. F.
Darnley, M. J.
Delgado, L.
Drake, J. J.
Hernanz, M.
Mukai, K.
Nelson, T.
Ness, J. U.
Schwarz, G. J.
Shore, S. N.
Starrfield, S.
Woodward, C. E.
First Published: 17-Oct-2015
Publisher: Oxford University Press (OUP)
Citation: Monthly Notices Of The Royal Astronomical Society, 2015, 454(3), pp. 3108-3120
Abstract: V745 Sco is a recurrent nova, with the most recent eruption occurring in February 2014. V745 Sco was first observed by Swift a mere 3.7 hr after the announcement of the optical discovery, with the super-soft X-ray emission being detected around four days later and lasting for only ~two days, making it both the fastest follow-up of a nova by Swift and the earliest switch-on of super-soft emission yet detected. Such an early switch-on time suggests a combination of a very high velocity outflow and low ejected mass and, together with the high effective temperature reached by the super-soft emission, a high mass white dwarf (>1.3 M_sun). The X-ray spectral evolution was followed from an early epoch where shocked emission was evident, through the entirety of the super-soft phase, showing evolving column density, emission lines, absorption edges and thermal continuum temperature. UV grism data were also obtained throughout the super-soft interval, with the spectra showing mainly emission lines from lower ionization transitions and the Balmer continuum in emission. V745 Sco is compared with both V2491 Cyg (another nova with a very short super-soft phase) and M31N 2008-12a (the most rapidly recurring nova yet discovered). The longer recurrence time compared to M31N 2008-12a could be due to a lower mass accretion rate, although inclination of the system may also play a part. Nova V745 Sco (2014) revealed the fastest evolving super-soft source phase yet discovered, providing a detailed and informative dataset for study.
DOI Link: 10.1093/mnras/stv2144
ISSN: 0035-8711
eISSN: 1365-2966
Version: Publisher Version
Status: Peer-reviewed
Type: Journal Article
Rights: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015 The Author. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. Deposited with reference to the publisher’s archiving policy available on the SHERPA/RoMEO website.
Description: 14 pages, 11 figures (4 in colour), accepted for publication in MNRAS
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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