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Authors: Schwarz, G. J.
Shore, S. N.
Page, K. L.
Osborne, Julian Paul
Beardmore, A. P.
Walter, F. M.
Bode, M. F.
Drake, J. J.
Ness, J-U.
Starrfield, S.
Van Rossum, D. R.
Woodward, C. E.
First Published: 9-Feb-2015
Publisher: IOP Publishing LTD
Citation: Astronomical Journal, 2015, 149 (3), 95
Abstract: We present the results of an intensive multiwavelength campaign on nova LMC 2012. This nova evolved very rapidly in all observed wavelengths. The time to fall two magnitudes in the V band was only 2 days. In X-rays the super soft phase began 13 ± 5 days after discovery and ended around day 50 after discovery. During the super soft phase, the Swift/XRT and Chandra spectra were consistent with the underlying white dwarf (WD) being very hot, ~1 MK, and luminous, ~10[Superscript: 38] erg s[Superscript: −1]. The UV, optical, and near-IR photometry showed a periodic variation after the initial and rapid fading had ended. Timing analysis revealed a consistent 19.24 ± 0.03 hr period in all UV, optical, and near-IR bands with amplitudes of ~0.3 mag which we associate with the orbital period of the central binary. No periods were detected in the corresponding X-ray data sets. A moderately high inclination system, i = 60 ± 10$^{{\circ{}}}$, was inferred from the early optical emission lines. The HST/STIS UV spectra were highly unusual with only the N v (1240 Å) line present and superposed on a blue continuum. The lack of emission lines and the observed UV and optical continua from four epochs can be fit with a low mass ejection event, ~10−6 ${{M}_{\odot }}$, from a hot and massive WD near the Chandrasekhar limit. The WD, in turn, significantly illuminated its subgiant companion which provided the bulk of the observed UV/optical continuum emission at the later dates. The inferred extreme WD characteristics and low mass ejection event favor nova LMC 2012 being a recurrent nova of the U Sco subclass.
DOI Link: 10.1088/0004-6256/149/3/95
ISSN: 0004-6256
eISSN: 1538-3881
Version: Publisher Version
Status: Peer-reviewed
Type: Journal Article
Rights: Copyright © 2015. The American Astronomical Society. All rights reserved. Deposited with reference to the publisher’s archiving policy available on the SHERPA/RoMEO website.
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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