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A remarkable recurrent nova in M31: Discovery and optical/UV observations of the predicted 2014 eruption
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SYSNO ASEP 0449357 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title A remarkable recurrent nova in M31: Discovery and optical/UV observations of the predicted 2014 eruption Author(s) Darnley, M.J. (GB)
Henze, M. (DE)
Steele, I.A. (GB)
Bode, M.F. (GB)
Ribeiro, V.A.R.M. (NL)
Rodriguez-Gil, P. (ES)
Shafter, A.W. (US)
Williams, S.C. (US)
Baer, D. (US)
Hachisu, I. (JP)
Hernanz, M. (ES)
Hornoch, Kamil (ASU-R) ORCID
Hounsell, R.A. (GB)
Kato, M. (JP)
Kiyota, S. (JP)
Kučáková, H. (CZ)
Maehara, H. (JP)
Ness, J.-U. (ES)
Piascik, A.S. (US)
Sala, G. (DE)
Skillen, I. (ES)
Smith, R. J. (US)
Wolf, M. (CZ)Source Title Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
Roč. 580, August (2015), A45/1-A45/23Number of pages 23 s. Publication form Online - E Language eng - English Country FR - France Keywords individual (M31) galaxies ; novae ; cataclysmic variables Subject RIV BN - Astronomy, Celestial Mechanics, Astrophysics OECD category Astronomy (including astrophysics,space science) Institutional support ASU-R - RVO:67985815 UT WOS 000360020200045 DOI 10.1051/0004-6361/201526027 Annotation Here we report the results of a high cadence multi-colour optical monitoring campaign, the spectroscopic evolution, and the UV photometry. We also discuss tantalising evidence of a potentially related, vastly-extended, nebulosity. The 2014 eruption was discovered, before optical maximum, on October 2, 2014. We find that the optical properties of M31N 2008-12a evolve faster than all Galactic recurrent novae known, and all its eruptions show remarkable similarity both photometrically and spectroscopically. Optical spectra were obtained as early as 0.26 days post maximum, and again confirm the nova nature of the eruption. A significant deceleration of the inferred ejecta expansion velocity is observed which may be caused by interaction of the ejecta with surrounding material, possibly a red giant wind. We find a low ejected mass and low ejection velocity, which are consistent with high mass-accretion rate, high mass white dwarf, and short recurrence time models of novae. We encourage additional observations, especially around the predicted time of the next eruption, towards the end of 2015. Workplace Astronomical Institute Contact Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Year of Publishing 2016
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