HS 2331+3905 : the cataclysmic variable that has it all
S. Araujo-Betancor,Boris T. Gänsicke,H. J. Hagen,T. R. Marsh,E. T. Harlaftis,John R. Thorstensen,R. E. Fried,P. Schmeer,D. Engels +8 more
TLDR
In this paper, the authors report detailed follow-up observations of the cataclysmic variable HS 2331+3905, identified as an emissionline object in the Hamburg Quasar Survey.Abstract:
We report detailed follow-up observations of the cataclysmic variable HS 2331+3905, identified as an emissionline object in the Hamburg Quasar Survey. An orbital period of 81.08 min is unambiguously determined from the detection of eclipses in the light curves of HS 2331+3905. A second photometric period is consistently detected at P
83.38 min,∼2.8% longer than P orb , which we tentatively relate to the presence of permanent superhumps. High time resolution photometry exhibits short-timescale variability on time scales of 5−6 min which we interpret as non-radial white dwarf pulsations, as well as a coherent signal at 1.12 min, which is likely to be the white dwarf spin period. A large-amplitude quasi-sinusoidal radial
velocity modulation of the Balmer and Helium lines with a period ∼3.5 h is persistently detected throughout three seasons of time-resolved spectroscopy. However, this spectroscopic period, which is in no way related to the orbital period, is not strictly coherent but drifts in period and/or phase on time scales of a few days. Modeling the far-ultraviolet to infrared spectral energy
distribution of HS 2331+3905, we determine a white dwarf temperature of T eff 10 500 K (assuming M wd = 0.6 M ), close to the ZZ Ceti instability strip of single white dwarfs. The spectral model implies a distance of d = 90 ± 15 pc, and a low value for the distance is supported by the large proper motion of the system, µ = 0.14 yr −1 . The non-detection of molecular bands and the low J, H, and K fluxes of HS 2331+3905 make this object a very likely candidate for a brown-dwarf donor.read more
Citations
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Magnetic White Dwarfs
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SDSS unveils a population of intrinsically faint cataclysmic variables at the minimum orbital period
Boris T. Gänsicke,Monihar Dillon,John Southworth,John R. Thorstensen,Pablo Rodríguez-Gil,A. Aungwerojwit,A. Aungwerojwit,Tom Marsh,Paula Szkody,S. C. C. Barros,Jorge Casares,D. de Martino,Paul J. Groot,Pasi Hakala,Ulrich Kolb,S. P. Littlefair,I. G. Martínez-Pais,I. G. Martínez-Pais,Gijs Nelemans,Matthias R. Schreiber +19 more
TL;DR: In this paper, the authors discuss the properties of 137 cataclysmic variables (CVs) which are included in the Sloan Digital Sky Survey (SDSS) spectroscopic data base, and for which accurate orbital periods have been measured.
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Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae
Taichi Kato,Akira Imada,Makoto Uemura,Daisaku Nogami,Hiroyuki Maehara,Ryoko Ishioka,Hajime Baba,Katsura Matsumoto,Hidetoshi Iwamatsu,Kaori Kubota,Kei Sugiyasu,Yuichi Soejima,Y. Moritani,Tomohito Ohshima,Hiroyuki Ohashi,Junpei Tanaka,Mahito Sasada,Akira Arai,Kazuhiro Nakajima,Seiichiro Kiyota,Kenji Tanabe,Kayuyoshi Imamura,Nanae Kunitomi,Kenji Kunihiro,Hiroki Taguchi,Mitsuo Koizumi,Norimi Yamada,Yuichi Nishi,Mayumi Kida,Sawa Tanaka,Rie Ueoka,Hideki Yasui,Koichi Maruoka,Arne Henden,Arto Oksanen,Marko Moilanen,Petri Tikkanen,Mika Aho,Berto Monard,Hiroshi Itoh,Pavol A. Dubovsky,Igor Kudzej,Radka Dancikova,Tonny Vanmunster,Jochen Pietz,Greg Bolt,David Boyd,Peter Nelson,Thomas Krajci,Lewis M. Cook,Ken'ichi Torii,Donn R. Starkey,Jeremy Shears,Lasse-Teist Jensen,Gianluca Masi,Rudolf Novak,Tomas Hynek,R. Kocián,Lukas Kral,H. Kucakova,Marek Kolasa,Petr Stastny,Bart Staels +62 more
TL;DR: In this article, period variations of superhumps in SU UMa-type dwarf novae based on newly obtained data and past publications were systematically surveyed and the evolution of the superhump period was found to be composed of three distinct stages: early evolutionary stage with a longer superhup period, middle stage with systematically varying periods, and final stage with shorter, stable superhum period.
Journal ArticleDOI
Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae
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TL;DR: In this article, period variations of superhumps in SU UMa-type dwarf novae based on newly obtained data and past publications were systematically surveyed and the evolution of the superhump period was found to be composed of three distinct stages: early evolutionary stage with a longer superhup period, middle stage with systematically varying periods, and final stage with shorter, stable superhum period.
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