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

2015 ◽  
Vol 2 (1) ◽  
pp. 123-127 ◽  
Author(s):  
N. Katysheva ◽  
S. Shugarov ◽  
N. Borisov ◽  
M. Gabdeev ◽  
P. Golysheva
Keyword(s):  
Spectroscopic Investigation ◽  
Short Review ◽  
Cataclysmic Variable ◽  
Dwarf Nova ◽  
Spectroscopic Observations ◽  
Photometric And Spectroscopic Observations

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

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

1996 ◽  
Vol 158 ◽  
pp. 73-74
Author(s):  
Irina Voloshina
Keyword(s):  
Cataclysmic Variable ◽  
Optical Monitoring ◽  
X Ray ◽  
Dwarf Nova ◽  
Spectroscopic Observations ◽  
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.

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 Photometric and Spectroscopic Observations of the Cataclysmic Variable AC Cancri

1983 ◽  
Vol 72 ◽  
pp. 17-20
Author(s):  
M. Kitamura ◽  
A. Okazaki ◽  
A. Yamasaki
Keyword(s):  
Astronomical Observatory ◽  
Light Curves ◽  
Cataclysmic Variable ◽  
Image Tube ◽  
Spectroscopic Observations ◽  
Photometric And Spectroscopic Observations

ABSTRACTThe eclipsing variable AC Cancri, recently identified as a cataclysmic variable by Shugarov (1981) and Okazaki, Kitamura and Yamasaki (1982), was further studied in detail on the bases of UBVcolours, multi-channel photoelectric light curves and image-tube spectrograms which were newly obtained at Tokyo Astronomical Observatory. The result of analysis of these materials for the nature of the cataclysmic variable is presented.

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

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 ◽  
Spectroscopic Observations ◽  
The Third ◽  
Photometric And Spectroscopic Observations

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.

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

2014 ◽  
Vol 9 (S307) ◽  
pp. 222-223
Author(s):  
D. Moździerski ◽  
Z. Kołaczkowski ◽  
E. Zahajkiewicz
Keyword(s):  
Seismic Modeling ◽  
Preliminary Results ◽  
Spectroscopic Observations ◽  
Seismic Modelling ◽  
Photometric And Spectroscopic Observations

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.

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

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 ◽  
Spectroscopic Observations ◽  
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%.

scholarly journals New photometric and spectroscopic observations of the Seyfert galaxy Mrk 315

2005 ◽  
Vol 360 (1) ◽  
pp. 253-271 ◽  
Author(s):  
S. Ciroi ◽  
V. L. Afanasiev ◽  
A. V. Moiseev ◽  
V. Botte ◽  
F. Di Mille ◽  
...  
Keyword(s):  
Seyfert Galaxy ◽  
Spectroscopic Observations ◽  
Photometric And Spectroscopic Observations
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