scholarly journals An IUE Archival Study of the White Dwarf Temperature Variation in the Dwarf Nova WZ Sagittae

2000 ◽  
Vol 9 (2) ◽  
Author(s):  
R. J. Slevinsky ◽  
D. Stys ◽  
S. West ◽  
E. M. Sion ◽  
F. H. Cheng
Keyword(s):  
Temperature Variation ◽  
White Dwarf ◽  
Dwarf Nova ◽  
Archival Study

scholarly journals A Far Ultraviolet Archival Study of Cataclysmic Variables. I.FUSEandHSTSTIS Spectra of the Exposed White Dwarf in Dwarf Nova Systems

2008 ◽  
Vol 679 (2) ◽  
pp. 1447-1466 ◽  
Author(s):  
Patrick Godon ◽  
Edward M. Sion ◽  
Paul E. Barrett ◽  
Ivan Hubeny ◽  
Albert P. Linnell ◽  
...  
Keyword(s):  
White Dwarf ◽  
Cataclysmic Variables ◽  
Dwarf Nova ◽  
Far Ultraviolet ◽  
Archival Study

scholarly journals [ITAL]Hubble Space Telescope[/ITAL] Observations of the Dwarf Nova WZ Sagittae: A Very Rapidly Rotating White Dwarf

1997 ◽  
Vol 484 (2) ◽  
pp. L149-L152 ◽  
Author(s):  
F. H. Cheng ◽  
Edward M. Sion ◽  
Paula Szkody ◽  
Min Huang
Keyword(s):  
White Dwarf ◽  
Hubble Space Telescope ◽  
Space Telescope ◽  
Dwarf Nova

scholarly journals Preliminary analysis of a Hubble FOS spectrum of VW Hyi in quiescence: A DAZQ white dwarf and accretion belt/ring

1996 ◽  
Vol 158 ◽  
pp. 249-250
Author(s):  
E. M. Sion ◽  
M. Huang ◽  
F. H. Cheng ◽  
I. Hubeny ◽  
P. Szkody
Keyword(s):  
White Dwarf ◽  
Preliminary Analysis ◽  
Hubble Space Telescope ◽  
Uv Spectrum ◽  
Space Telescope ◽  
Dwarf Nova ◽  
Faint Object ◽  
Faint Object Spectrograph

AbstractWe present a preliminary analysis of the UV spectrum of the dwarf nova VW Hyi during early quiescence, obtained with the Faint Object Spectrograph (FOS) on the Hubble Space Telescope (HST). The data were obtained approximately one day after the end of a normal outburst.

scholarly journals Superoutbursts and Superhumps of SU UMa Stars

1988 ◽  
Vol 108 ◽  
pp. 238-239
Author(s):  
Yoji Osaki ◽  
Masahito Hirose
Keyword(s):  
Accretion Disk ◽  
Orbital Period ◽  
White Dwarf ◽  
Binary Systems ◽  
Roche Lobe ◽  
Light Curves ◽  
Close Binary ◽  
Dwarf Novae ◽  
Dwarf Nova ◽  
Close Binary Systems

SU UMa stars are one of subclasses of dwarf novae. Dwarf novae are semi-detached close binary systems in which a Roche-lobe filling red dwarf secondary loses matter and the white dwarf primary accretes it through the accretion disk. The main characteristics of SU UMa subclass is that they show two kinds of outbursts: normal outbursts and superoutbursts. In addition to the more frequent narrow outbursts of normal dwarf nova, SU UMa stars exhibit “superoutbursts”, in which stars reach about 1 magnitude brighter and stay longer than in normal outburst. Careful photometric studies during superoutburst have almost always revealed the “superhumps”: periodic humps in light curves with a period very close to the orbital period of the system. However, the most curious of all is that this superhump period is not exactly equal to the orbital period, but it is always longer by a few percent than the orbital period.

A Hubble Space Telescope study of the underlying white dwarf in the dwarf nova VW Hydri during quiescence

1995 ◽  
Vol 444 ◽  
pp. L97 ◽  
Author(s):  
Edward M. Sion ◽  
Paula Szkody ◽  
Fu-Hua Cheng ◽  
Min Huang
Keyword(s):  
White Dwarf ◽  
Hubble Space Telescope ◽  
Space Telescope ◽  
Dwarf Nova

scholarly journals Pulsating white dwarfs in cataclysmic variables: The marriage of ZZ Cet and dwarf nova

2004 ◽  
Vol 193 ◽  
pp. 382-386 ◽  
Author(s):  
Brian Warner ◽  
Patrick A. Woudt
Keyword(s):  
White Dwarf ◽  
Large Amplitude ◽  
White Dwarfs ◽  
Cataclysmic Variables ◽  
Sloan Digital Sky Survey ◽  
Dwarf Novae ◽  
Dwarf Nova ◽  
Sky Survey

AbstractThere are now four dwarf novae known with white dwarf primaries that show large amplitude non-radial oscillations of the kind seen in ZZ Cet stars. We compare the properties of these stars and point out that by the end of the Sloan Digital Sky Survey more than 30 should be known.

The Dwarf Nova EX Hydrae

1974 ◽  
Vol 2 (5) ◽  
pp. 271-274 ◽  
Author(s):  
R. D. Watson ◽  
P. T. Rayner
Keyword(s):  
Binary System ◽  
Time Resolution ◽  
White Dwarf ◽  
Roche Lobe ◽  
Dwarf Star ◽  
Dwarf Nova ◽  
Photoelectric Time

The object EX Hya is a dwarf nova with a binary period of 98.3 min (Mumford 1964, 1967). Warner (1972, 1973a) has observed two complete cycles of this star with a photoelectric time resolution of 5 sec. These observations suggested that EX Hya can be understood in terms of the model proposed by Warner and Nather (1971) in their discussion of U Gem. In this model, a white dwarf primary of a semi-detached binary system is surrounded by a disk of gas formed from matter transfered from the secondary, which is a cool dwarf star filling its Roche lobe.

scholarly journals A Wave Model for Dwarf Novae

1980 ◽  
Vol 58 ◽  
pp. 643-648
Author(s):  
Warren M. Sparks ◽  
G. Siegfried Kutter
Keyword(s):  
Binary System ◽  
White Dwarf ◽  
Wave Model ◽  
Mathematical Representation ◽  
Coherent Oscillation ◽  
Dwarf Novae ◽  
Dwarf Nova ◽  
Nova Outburst

AbstractThe rapid coherent oscillation during a dwarf nova outburst is attributed to an accretion-driven wave going around the white dwarf component of the binary system. The increase and decrease in the period of this oscillation is due to the change in the velocity of the wave as it is first being driven and then damped. Qualitatively, a large number of observations can be explained with such a model. The beginnings of a mathematical representation of this model are developed.

scholarly journals An ASCA Observation of the Eclipsing Dwarf Nova HT Cas

1996 ◽  
Vol 158 ◽  
pp. 269-272
Author(s):  
K. Mukai ◽  
E. M. Schlegel ◽  
J. H. Swank ◽  
T. Naylor ◽  
Janet H. Wood
Keyword(s):  
Boundary Layer ◽  
White Dwarf ◽  
X Rays ◽  
X Ray ◽  
Dwarf Nova

AbstractWe report on a 1-day ASCA observation of the eclipsing dwarf nova HT Cas. We confirm the presence of an X-ray eclipse, which is narrow and deep. The data are consistent with the X-rays originating entirely from the immediate neighborhood of the white dwarf. We draw some preliminary conclusions on the boundary layer and other relevant issues.

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