Mass distribution of DA white dwarfs

1984 ◽  
Vol 100 (1-2) ◽  
pp. 471-473 ◽  
Author(s):  
D. Koester
Keyword(s):  
Mass Distribution ◽  
White Dwarfs

The Temperature Scale and Mass Distribution of Hot DA White Dwarfs

1997 ◽  
Vol 488 (1) ◽  
pp. 375-396 ◽  
Author(s):  
David S. Finley ◽  
Detlev Koester ◽  
Gibor Basri
Keyword(s):  
Mass Distribution ◽  
White Dwarfs ◽  
Temperature Scale

Atmospheric parameters and mass distribution of DA-white dwarfs

1983 ◽  
Vol 96 (1) ◽  
pp. 1-23 ◽  
Author(s):  
O. H. Guseinov ◽  
H. I. Novruzova ◽  
Y. S. Rustamov
Keyword(s):  
Mass Distribution ◽  
White Dwarfs ◽  
Atmospheric Parameters

scholarly journals A Comparative Study of the Mass Distribution of Extreme‐Ultraviolet–selected White Dwarfs

1999 ◽  
Vol 517 (1) ◽  
pp. 399-415 ◽  
Author(s):  
R. Napiwotzki ◽  
Paul J. Green ◽  
Rex A. Saffer
Keyword(s):  
Comparative Study ◽  
Mass Distribution ◽  
White Dwarfs ◽  
Extreme Ultraviolet

scholarly journals Mass Distribution and Luminosity Function of White Dwarfs

1989 ◽  
Vol 114 ◽  
pp. 1-14 ◽  
Author(s):  
Volker Weidemann ◽  
Jie W. Yuan
Keyword(s):  
Mass Loss ◽  
Mass Distribution ◽  
Stellar Evolution ◽  
White Dwarf ◽  
White Dwarfs ◽  
Luminosity Function ◽  
Present Situation ◽  
Single Well ◽  
Mass Dispersion

Ever since Graham’s Strömgren photometry (1972) demonstrated the existence of a single well defined cooling sequence of DA white dwarfs the question of the mass dispersion (or the width of the number-mass distribution) has been in the foreground of my studies (Weidemann, 1970, 1977).Indeed it turned out that the shape of the white dwarf mass distribution provides strong constraints on the theory of stellar evolution with mass loss, a fact which will be demonstrated again in the following lecture. It therefore seems worthwhile to dwell in some detail on the methods of its determination. For the benefit of the non-specialists I shall first present some of the historical results and then continue to discuss the present situation.

scholarly journals The White Dwarf Mass and Orbital Period Distributions in Zero-Age Cataclysmic Variables

1990 ◽  
Vol 122 ◽  
pp. 392-393
Author(s):  
M. Politano ◽  
R.F. Webbink
Keyword(s):  
Mass Distribution ◽  
White Dwarf ◽  
White Dwarfs ◽  
Stellar Population ◽  
Cataclysmic Variables ◽  
Cataclysmic Variable ◽  
Solar Mass ◽  
Orbital Periods ◽  
Rapid Mass ◽  
Made In

A zero-age cataclysmic variable (ZACV) we define as a binary system at the onset of interaction as a cataclysmic variable. We present here the results of calculations of the distributions of white dwarf masses and of orbital periods in ZACVs, due to binaries present in a stellar population which has undergone continuous, constant star formation for 1010 years. These results differ from previous work (Politano and Webbink 1988) in that an improved criterion for stability against rapid mass transfer by the secondary to the white dwarf has been used. A brief outline of the method and key assumptions made in this calculation is given in Politano and Webbink (1988).The white dwarf mass distribution of ZACVs (shown in Figure 1) contains two components: systems with helium white dwarfs and systems with C-0 white dwarfs. Systems with helium white dwarfs comprise slightly greater than 50% of all ZACVs. The helium white dwarfs have masses which range from 0.27 to 0.46 solar mass. The C-0 white dwarfs have masses which range from 0.54 solar mass up to the Chandrasekhar mass. (Note: systems with O-Ne-Mg white dwarfs are not distinguished from systems with C-0 white dwarfs in this calculation. Presumably, these O-Ne-Mg systems comprise the upper end of the white dwarf mass distribution.)

A spectroscopic determination of the mass distribution of DA white dwarfs

1992 ◽  
Vol 394 ◽  
pp. 228 ◽  
Author(s):  
P. Bergeron ◽  
Rex A. Saffer ◽  
James Liebert
Keyword(s):  
Mass Distribution ◽  
White Dwarfs ◽  
Spectroscopic Determination
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