On the Formation of O-Ne White Dwarfs in Metal-rich Close Binary Systems

1993 ◽  
Vol 419 ◽  
pp. 268 ◽  
Author(s):  
Inma Dominguez ◽  
Amedeo Tornambe ◽  
Jordi Isern
Keyword(s):  
White Dwarfs ◽  
Binary Systems ◽  
Close Binary ◽  
Close Binary Systems

scholarly journals Nucleosynthesis During Nova Explosions and Grain Formations in Ejected Envelopes

1979 ◽  
Vol 53 ◽  
pp. 533-533
Author(s):  
Masayuki Y. Fujimoto
Keyword(s):  
General Theory ◽  
White Dwarf ◽  
White Dwarfs ◽  
Binary Systems ◽  
Thermal Emission ◽  
Finite Amplitude ◽  
Close Binary ◽  
Close Binary Systems

Recent observations have revealed the existence of infrared brightening in some nova explosions, and its absence in others. These infrared excesses are ascribed to thermal emission from grains which are considered to consist of graphite. Such nova explosions are widely accepted to be triggered by hydrogen shell-flashes on the surface of white dwarfs which accrete matter in close binary systems. As for the hydrogen shell-flash, recently, a general theory applicable even to the case of finite amplitude has been developed. According to this theory, the progress of a shell-flash is determined only by the mass of the white dwarf MWD and the mass of the accreted hydrogen-rich envelope ΔMH.

scholarly journals m = 1 Oscillations of Accretion Disks in Close Binary Systems

1997 ◽  
Vol 163 ◽  
pp. 777-778
Author(s):  
Atsuo T. Okazaki
Keyword(s):  
Accretion Disks ◽  
Fundamental Mode ◽  
White Dwarfs ◽  
Binary Systems ◽  
Close Binary ◽  
Dimensional Structure ◽  
Two Dimensional ◽  
Close Binary Systems

AbstractWe examine the two-dimensional structure of m = 1 modes in disks around white dwarfs in close binary systems. We find that the odd modes (warping modes) as well as even modes (eccentric modes) are confined to the outermost part of the disk. The period of the fundamental mode is of a few percent of the binary period, and is insensitive to the parity of the mode. These modes naturally explain the superhump periods of SU UMa stars.

scholarly journals Explosion of White Dwarfs

1987 ◽  
Vol 93 ◽  
pp. 413-417
Author(s):  
R. Lopez ◽  
J. Isern ◽  
J. Labay ◽  
R. Canal
Keyword(s):  
Light Curve ◽  
White Dwarfs ◽  
Binary Systems ◽  
Light Curves ◽  
Close Binary ◽  
Classical Type ◽  
Type I ◽  
Close Binary Systems ◽  
Systems Studies

AbstractWe present models for Type I supernova light curves based on the explosion of partially solid white dwarfs in close binary systems. Studies of such explosions show that they leave bound remnants of different size. Our results reproduce quite well the maximun luminosities, the expansion velocities and the shape of the light curve. As the two basic papameters that govern the light curve, the ejected mass and the mass of 56Ni produced, are variable our models reproduce the slow and fast subclasses of “classical” Type I supernovae.

scholarly journals New Close Binary Systems from the SDSS-I (Data Release Five) and the Search for Magnetic White Dwarfs in Cataclysmic Variable Progenitor Systems

2007 ◽  
Vol 134 (2) ◽  
pp. 741-748 ◽  
Author(s):  
Nicole M. Silvestri ◽  
Mara P. Lemagie ◽  
Suzanne L. Hawley ◽  
Andrew A. West ◽  
Gary D. Schmidt ◽  
...  
Keyword(s):  
White Dwarfs ◽  
Binary Systems ◽  
Close Binary ◽  
Cataclysmic Variable ◽  
Close Binary Systems ◽  
Data Release

Some Results of the Spectroscopic Study of Four Close Binary Systems of Early Spectral Types

1965 ◽  
Vol 5 ◽  
pp. 120-130
Author(s):  
T. S. Galkina
Keyword(s):  
Spectroscopic Study ◽  
Spectral Type ◽  
Spectroscopic Investigation ◽  
Binary Systems ◽  
Quantitative Information ◽  
Close Binary ◽  
Physical Parameters ◽  
Absorption And Emission ◽  
Close Binary Systems ◽  
Quantitative Estimates

It is necessary to have quantitative estimates of the intensity of lines (both absorption and emission) to obtain the physical parameters of the atmosphere of components.Some years ago at the Crimean observatory we began the spectroscopic investigation of close binary systems of the early spectral type with components WR, Of, O, B to try and obtain more quantitative information from the study of the spectra of the components.

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