Models of Cataclysmic Variables from Photometric and Spectroscopic Data

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.

Photometric and Spectroscopic Investigation of the Dwarf Nova HS 0218+3229: A Short Review

Acta Polytechnica CTU Proceedings ◽

10.14311/app.2015.02.0123 ◽

2015 ◽

Vol 2 (1) ◽

pp. 123-127 ◽

Cited By ~ 2

Author(s):

N. Katysheva ◽

S. Shugarov ◽

N. Borisov ◽

M. Gabdeev ◽

P. Golysheva

Keyword(s):

Spectroscopic Investigation ◽

Short Review ◽

Cataclysmic Variable ◽

Dwarf Nova ◽

This paper is devoted to the study of the cataclysmic variable HS 0218+3229 using the photometric and spectroscopic observations.

Binary Stars among Cataclysmic Variables. XI. Photoelectric and Spectroscopic Observations of the Dwarf Nova Z Camelopardalis

The Astrophysical Journal ◽

10.1086/150220 ◽

1969 ◽

Vol 158 ◽

pp. 589 ◽

Cited By ~ 18

Author(s):

Robert P. Kraft ◽

W. Krzeminski ◽

George S. Mumford

Keyword(s):

Binary Stars ◽

Cataclysmic Variables ◽

Dwarf Nova ◽

Spectroscopic Observations

Results of Optical Monitoring of the Dwarf Nova SS Cyg During the 1993 Campaign of co-ordinated Observations with the Asca Satellite

International Astronomical Union Colloquium ◽

10.1017/s0252921100038252 ◽

1996 ◽

Vol 158 ◽

pp. 73-74

Author(s):

Irina Voloshina

Keyword(s):

Cataclysmic Variable ◽

Optical Monitoring ◽

X Ray ◽

Dwarf Nova ◽

Photometric And Spectroscopic Observations ◽

Wide Range

SS Cyg is the brightest known and therefore best studied classical dwarf nova and it was the first one from which X-ray radiation was discovered. SS Cyg is unique because it has been detected at very wide range of energies, from a few eV up to ~ 10 keV (Jones & Watson 1992). It was chosen as the first cataclysmic variable for X-ray observations with the Japanese satellite ASCA. Simultaneous optical photometric and spectroscopic observations were also provided for completeness of the study.

First detection of two superoutbursts during the rebrightening phase of a WZ Sge-type dwarf nova: TCP J21040470+4631129

Publications of the Astronomical Society of Japan ◽

10.1093/pasj/psaa043 ◽

2020 ◽

Vol 72 (3) ◽

Author(s):

Yusuke Tampo ◽

Kojiguchi Naoto ◽

Keisuke Isogai ◽

Taichi Kato ◽

Mariko Kimura ◽

...

Keyword(s):

Mass Transfer ◽

Accretion Disk ◽

Late Stage ◽

Large Radius ◽

Mass Ratio ◽

Dwarf Novae ◽

Dwarf Nova ◽

The Third ◽

Abstract We report on photometric and spectroscopic observations and analysis of the 2019 superoutburst of TCP J21040470+4631129. This object showed a 9 mag superoutburst with early superhumps and ordinary superhumps, which are the features of WZ Sge-type dwarf novae. Five rebrightenings were observed after the main superoutburst. The spectra during the post-superoutburst stage showed Balmer, He i, and possible sodium doublet features. The mass ratio is derived as 0.0880(9) from the period of the superhump. During the third and fifth rebrightenings, growing superhumps and superoutbursts were observed, which have never been detected during a rebrightening phase among WZ Sge-type dwarf novae with multiple rebrightenings. To induce a superoutburst during the brightening phase, the accretion disk needs to have expanded beyond the 3 : 1 resonance radius of the system again after the main superoutburst. These peculiar phenomena can be explained by the enhanced viscosity and large radius of the accretion disk suggested by the higher luminosity and the presence of late-stage superhumps during the post-superoutburst stage, plus by more mass supply from the cool mass reservoir and/or from the secondary because of the enhanced mass transfer than those of other WZ Sge-type dwarf novae.

Photometric and spectroscopic observations of the old nova T Aur

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/192.2.127 ◽

1980 ◽

Vol 192 (2) ◽

pp. 127-134 ◽

Cited By ~ 5

Author(s):

A. Bianchini

Keyword(s):

An attempt of seismic modelling of β Cephei stars in NGC 6910

Proceedings of the International Astronomical Union ◽

10.1017/s1743921314006796 ◽

2014 ◽

Vol 9 (S307) ◽

pp. 222-223

Author(s):

D. Moździerski ◽

Z. Kołaczkowski ◽

E. Zahajkiewicz

Keyword(s):

Seismic Modeling ◽

Preliminary Results ◽

Seismic Modelling ◽

AbstractWe present preliminary results of seismic modeling of β Cephei-type stars in NGC 6910 based on simultaneous photometric and spectroscopic observations carried out in 2013 in Białków (photometry) and Apache Point (spectroscopy) observatories.

V 3903 Sagitarii: A Main-Sequence (07V+09V) Detached Eclipsing Binary

International Astronomical Union Colloquium ◽

10.1017/s025292110001808x ◽

1993 ◽

Vol 137 ◽

pp. 371-373

Author(s):

L.P.R. Vaz ◽

N.C.S. Cunha ◽

E.F. Vieira ◽

M.L.M. Myrrha

Keyword(s):

Main Sequence ◽

Eclipsing Binary ◽

Photometric And Spectroscopic Observations ◽

Absolute Dimensions

AbstractPhotometric and spectroscopic observations of V3903 Sgr are analyzed, and absolute dimensions (masses and radii) are determined to a precision better then 3%.