Photometric Determination of Orbital Inclinations and Mass Loss Rates for Wolf-Rayet Stars in WR+O Binaries

1996 ◽  
Vol 112 ◽  
pp. 2227 ◽  
Author(s):  
Robert Lamontagne ◽  
Anthony F. J. Moffat ◽  
Laurent Drissen ◽  
Carmelle Robert ◽  
Jaymie M. Matthews
Keyword(s):  
Mass Loss ◽  
Photometric Determination ◽  
Loss Rates

Photometric Determination of Mass Loss Rates and Orbital Inclinations for WR Binaries

1991 ◽  
pp. 316-316
Author(s):  
R. Lamontagne ◽  
C. Robert ◽  
A. Grandchamps ◽  
N. Lapierre ◽  
A. Moffat ◽  
...  
Keyword(s):  
Mass Loss ◽  
Photometric Determination ◽  
Loss Rates

scholarly journals Photometric Determination of Mass Loss Rates and Orbital Inclinations for WR Binaries

1991 ◽  
Vol 143 ◽  
pp. 316-316
Author(s):  
R. Lamontagne ◽  
C. Robert ◽  
A. Grandchamps ◽  
N. Lapierre ◽  
A. Moffat ◽  
...  
Keyword(s):  
Simple Model ◽  
Mass Loss ◽  
Electron Scattering ◽  
Orbital Period ◽  
Photometric Determination ◽  
Spherically Symmetric ◽  
Loss Rates

Most Wolf-Rayet binaries show phase-dependent light variations with a broad dip occurring at phase zero, when the WR star passes closest to the observer. When the orbital period is long, or the inclination is low, this dip is buried in the noise. When eclipses of the stars occur, another dip is seen when the companion passes closest to the observer; in this case, both dips are relatively deep and sharp (e.g. V444 Cygni, HD5980).In the cases when only one dip at phase zero is seen, a simple model is derived. This involves electron scattering of companion starlight as the orbit makes it systematically traverse different amounts of the WR wind, assumed to be spherically symmetric and to follow a monotonic velocity-radius law. The shape and amplitude of the dip yield estimates of M and i (hence M when combined with M sin3i from spectroscopic orbits).

scholarly journals The Ionization in the Winds of O Stars and the Determination of Mass‐Loss Rates from Ultraviolet Lines

1999 ◽  
Vol 516 (2) ◽  
pp. 872-886 ◽  
Author(s):  
Henny J. G. L. M. Lamers ◽  
Stephan Haser ◽  
Alex de Koter ◽  
Claus Leitherer
Keyword(s):  
Mass Loss ◽  
Loss Rates

scholarly journals The Influence of the Ratio of Total to Selective Extinction on the Determination of the Mass Loss Rate of Wolf Rayet Stars from Infrared Excess Measurements

1982 ◽  
Vol 99 ◽  
pp. 197-201
Author(s):  
P.S. The ◽  
K.A. van der Hucht ◽  
M. Arens
Keyword(s):  
Mass Loss ◽  
Loss Rate ◽  
Near Infrared ◽  
Mass Loss Rate ◽  
Infrared Excess ◽  
Photometric Observations ◽  
Order Of Magnitude ◽  
Selective Extinction ◽  
Loss Rates

It is shown that the mass loss rate of the WN7 star HD 93162 decreases with larger values of the ratio of total to selective extinction R. for HD 93162 the mass loss rate will change one order of magnitude, only if ΔR ∼ 2. Mass loss rates are derived for nine other WR stars of which visual, red and near-infrared photometric observations were obtained.

Estimation of Mass-loss Rates for Some Galactic Wolf Rayet Stars

1991 ◽  
Vol 9 (2) ◽  
pp. 275-276
Author(s):  
Jong Ok Woo
Keyword(s):  
Mass Loss ◽  
Stellar Wind ◽  
Empirical Relation ◽  
Terminal Velocity ◽  
Effective Temperatures ◽  
The Absolute ◽  
Absolute Measurements ◽  
Loss Rates ◽  
Angular Diameters

AbstractThe absolute measurements of flux emitted in the visible continua of some Galactic Wolf-Rayet stars were carried out by means of a two-channel scanner. The measurements lead to the determination of stellar angular diameters which enable us to compute log L*/L⊙. The stellar wind terminal velocity, V∞ was obtained from the empirical relation of the effective temperatures by Underbill (1983) and V∞, adopted from the work of Willis (1982). Also, we derived the rate of mass loss for the WR stars from the formula Ṁ = є(Teff)L/(V∞c) by using the obtained effective temperatures, luminosity and V∞ in this work. The values of the rates range from 1.4 × 10−5 to 5.8 × 10−5M⊙yr−1.

scholarly journals Mass Loss Rates in Central Stars of Planetary Nebulae

1989 ◽  
Vol 131 ◽  
pp. 293-300 ◽  
Author(s):  
M. Perinotto
Keyword(s):  
Mass Loss ◽  
Planetary Nebulae ◽  
Central Star ◽  
Line Radiation ◽  
The Status ◽  
The Right ◽  
Central Stars ◽  
Loss Rates

Central stars of planetary nebulae (PNCS) frequently exhibit fast winds (cf. Cerruti-Sola and Perinotto, 1985; C.P. and Grewing, this volume). They may be important for the structure of the whole nebula as well as for the evolution of the central star. Their speed is typically two orders of magnitude higher than that of the classical optically visible nebula, which in turn expands a few times faster than the most external winds detected in few cases in the radio domain.I review here the status of art in the determination of the mass loss rates (M) associated with these fast winds. I restrict myself to the ‘observational’ determinations. Only at the end I will say something about the predictions of multi-scattering line radiation wind driven theory in connection with one best studied object: N6C 6543. This allows one to conclude that this theory may be the right explanation also for these winds.

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