scholarly journals IUE archive observations of dwarf nova WZ Sge during outburst

1989 ◽  
Vol 238 (2) ◽  
pp. 587-594 ◽  
Author(s):  
T. Naylor
Keyword(s):  
Dwarf Nova

Models of Cataclysmic Variables from Photometric and Spectroscopic Data

1979 ◽  
Vol 46 ◽  
pp. 65-74 ◽  
Author(s):  
A.C. Fabian ◽  
J.E. Pringle ◽  
J.A.J. Whelan ◽  
J.A. Bailey
Keyword(s):  
Spectroscopic Data ◽  
Cataclysmic Variables ◽  
System Parameters ◽  
Dwarf Nova ◽  
Spectroscopic Observations ◽  
Photometric And Spectroscopic Observations

Abstract.Recent photometric and spectroscopic observations of the dwarf nova system Z Cha are discussed. Methods for constraining the system parameters are applied and the disc emissivity is deduced as a function of radius. Indications are found that the disc shrinks in size with increasing time after outburst.

scholarly journals Erratum: OT J002656.6+284933 (CSS101212:002657+284933): an SUUMa-type dwarf nova with the longest superhump period

2017 ◽  
Vol 69 (3) ◽  
Author(s):  
Taichi Kato ◽  
Tamás Tordai ◽  
Colin Littlefield ◽  
Kiyoshi Kasai ◽  
Sergey Yu. Shugarov ◽  
...  
Keyword(s):  
Dwarf Nova

scholarly journals Photometric Observation of a New in-the-Gap SU UMa-Type Dwarf Nova V 725 Aquilae during the 1999 Superoutburst

2001 ◽  
Vol 53 (3) ◽  
pp. 539-546 ◽  
Author(s):  
Makoto Uemura ◽  
Taichi Kato ◽  
Elena Pavlenko ◽  
Alex Baklanov ◽  
Jochen Pietz
Keyword(s):  
Photometric Observation ◽  
Dwarf Nova

A Spectroscopic Study of the SU UMa-type Dwarf Nova YZ Cnc during its 2002 Superoutburst

2005 ◽  
Vol 5 (6) ◽  
pp. 601-609 ◽  
Author(s):  
Ying-He Zhao ◽  
Zong-Yun Li ◽  
Xiao-An Wu ◽  
Qiu-He Peng
Keyword(s):  
Spectroscopic Study ◽  
Dwarf Nova

scholarly journals The May 1985 Superoutburst of OY Carinae: II. Phase-Resolved IUE Spectroscopy and Exosat Observations

1987 ◽  
Vol 93 ◽  
pp. 371-376 ◽  
Author(s):  
B.J.M. Hassall ◽  
T. Naylor ◽  
G.T. Bath ◽  
P.A. Charles ◽  
G. Sonneborn ◽  
...  
Keyword(s):  
Emission Line ◽  
Line Spectrum ◽  
X Ray ◽  
Dwarf Nova ◽  
Uv Emission ◽  
Emission Line Spectrum ◽  
Coronal Region

AbstractWe present ultraviolet and X-ray observations of the eclipsing SU UMa dwarf nova OY Car early in the decline from a superoutburst. From the UV emission line spectrum and lack of X-ray eclipse, we deduce the presence of an extended coronal region.

scholarly journals UV Spectroscopy of the Novalike Variable TT Arietis

1982 ◽  
Vol 69 ◽  
pp. 453-454
Author(s):  
W. Wargau ◽  
H. Drechsel ◽  
J. Rahe ◽  
G. Klare ◽  
B. Wolf ◽  
...  
Keyword(s):  
Uv Spectroscopy ◽  
Wavelength Region ◽  
Apparent Magnitude ◽  
Long Wavelength ◽  
Dwarf Nova ◽  
Tt Ari ◽  
Visual Brightness

TT Ari was detected by Strohmeier et al. (1957) and is classified as a novalike variable. It was hitherto unclear whether TT Ari is a special type of dwarf nova (Warner, 1976) or an old nova (Cowley et al., 1975). Our group obtained a total of four IUE spectra between 1979 and 1981 in the short and long wavelength region. The first spectrum was taken in July 1979, when the system had a visual brightness of 11.3 magnitudes. The following two IUE observations in November 1980 revealed TT Ari in the lowest optical state (V = 14m.3) observed so far. The fourth spectrum was obtained during the rise to maximum in January 1981, when the system had an apparent magnitude of V = 11m.8. From this behavior, Krautter et al. (1981) concluded that TT Ari is a dwarf nova with extremely extended standstills as they are typical for Z Cam stars.

Simultaneous infrared and optical photometry of the Eclipsing Dwarf Nova V2051 Ophiuchi

1986 ◽  
Vol 6 (3) ◽  
pp. 306-308 ◽  
Author(s):  
D. J. Watts ◽  
R. D. Watson
Keyword(s):  
Light Curve ◽  
Optical Photometry ◽  
Dwarf Nova

AbstractA complete orbital light-curve of V2051 Oph in the IR H band is presented, together with a second eclipse in the J band. Simultaneous Rc band data were obtained. Eclipse depths in Rc, J and H are 1.8 mag, 1.0 mag and 0.8 mag respectively. No evidence for ellipsoidal variations due to the secondary was seen and constraints on the secondary are discussed.

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