scholarly journals Mass Loss and Shell Masses of Close Binary Stars

1987 ◽  
Vol 93 ◽  
pp. 675-679
Author(s):  
V.G. Karetnikov
Keyword(s):  
Mass Transfer ◽  
Mass Loss ◽  
Binary Stars ◽  
Transfer Rate ◽  
Mass Transfer Rate ◽  
Close Binary ◽  
Time Interval ◽  
Close Binary Stars

AbstractFrom the values of period changes for 6 close binary stars the mass transfer rate was calculated. Comparing these values Mt with the values of shell masses Msh, the expressionwas derived. The analysis of this expression points out the initial character of the outflow of matter, and one may determine the time interval of the substitution of the shell matter. So one may conclude that for a certain mass transfer rate, a certain amount of matter accumulates in the nearby regions of the system.

scholarly journals Close binary models for Luminous Blue Variable stars

1989 ◽  
Vol 113 ◽  
pp. 185-194
Author(s):  
J. S. Gallagher
Keyword(s):  
Mass Loss ◽  
Binary Stars ◽  
Mass Loss Rate ◽  
Variable Stars ◽  
High Mass ◽  
Close Binary ◽  
Close Binaries ◽  
System A ◽  
Close Binary Stars ◽  
High Mass Loss

AbstractThe evolution of massive close binary stars inevitably involves mass exchange between the two stellar components as well as mass loss from the system. A combination of these two processes could produce the stellar wind-modulated behavior seen in LB Vs. The possibility that LBVs are powered by accretion is examined, and does not appear to be a satisfactory general model. Instead, identification of LBVs with close binaries in high mass-loss rate or common envelope evolutionary phases shows promise.

scholarly journals Mass Transfer Characterization in Close Binary Stars

1992 ◽  
Vol 151 ◽  
pp. 337-340
Author(s):  
J. M. García ◽  
A. Giménez
Keyword(s):  
Mass Transfer ◽  
Angular Momentum ◽  
Binary Stars ◽  
Binary Star ◽  
Type System ◽  
Close Binary ◽  
Select Group ◽  
Close Binary Stars ◽  
Loss Of Mass ◽  
Close Binary Star

A method for estimating representative values of the parameters that characterize the loss of mass and angular momentum occurred during the evolution of a close binary star is considered. Absolute dimensions previous to mass-transfer stage have been obtained for a select group of 43 semidetached systems adopting a grid of values of mass loss, angular momentum loss and initial mass ratio. Our study reveals a highly non-conservative scenario for the evolution towards an Algol-type system.

scholarly journals Wind Driven Mass Transfer in Interacting Binaries

1992 ◽  
Vol 151 ◽  
pp. 363-366
Author(s):  
Christopher A. Tout ◽  
Douglas S. Hall
Keyword(s):  
Mass Transfer ◽  
Mass Loss ◽  
Binary Systems ◽  
Loss Rate ◽  
Mass Loss Rate ◽  
Mass Transfer Rate ◽  
Close Binary ◽  
Driving Mechanism ◽  
Simple Explanation ◽  
Quantitative Estimates

Stars in close binary systems can suffer two kinds of mass change: 1) mass transfer between the stars 2) mass loss completely from the system. Observational estimates indicate that these are of the same order. A simple explanation can be found if the mass loss, by stellar wind, from the Roche-filling star is the driving mechanism behind mass transfer. We find quantitative estimates for the necessary conditions and find that the mass transfer rate and the mass loss rate are indeed similar. We find that the radii of evolved semi-detached systems are more consistent with wind-driven evolution than the traditional nuclear-driven Roche-lobe overflow.

scholarly journals Mass loss from interacting close binary systems

1981 ◽  
Vol 59 ◽  
pp. 431-456
Author(s):  
Mirek J. Plavec
Keyword(s):  
Mass Transfer ◽  
Mass Loss ◽  
Binary Stars ◽  
Binary Systems ◽  
Close Binary ◽  
Important Process ◽  
Close Binary Systems ◽  
Complex Process ◽  
General Complex ◽  
Mass Outflow

AbstractMass outflow from interacting close binary systems, accompanied by loss of orbital angular momentum, appears to be a very important process affecting the evolution of binary stars. Together with accretion on the mass-gaining component, it is the least understood aspect of the general complex process we call “evolution with mass transfer and/or mass loss”, or, more briefly, “interaction”. It is therefore very imperative to assemble and examine all available facts or hints about mass loss.

scholarly journals Effective Growth Rate of White Dwarf Mass in Nova Outbursts

1990 ◽  
Vol 122 ◽  
pp. 390-391
Author(s):  
Mariko Kato ◽  
Izumi Hachisu
Keyword(s):  
Mass Transfer ◽  
Growth Rate ◽  
Mass Loss ◽  
White Dwarf ◽  
Transfer Rate ◽  
Mass Transfer Rate ◽  
Net Growth Rate ◽  
Chandrasekhar Limit ◽  
Nova Outbursts ◽  
Effective Growth

AbstractWe have obtained the effective growth rate of white dwarf masses which are suffering mass loss during both hydrogen and helium nova outbursts. If the mass transfer rate from the companion is smaller than 10−7 M⊙/yr, the net growth rate is reduced to less than one tenth of the mass transfer rate from the companion star. It is suggested that the white dwarf mass is hard to grow to the Chandrasekhar mass unless its initial mass is very close to the Chandrasekhar limit.

scholarly journals From Dinuclear Systems to Close Binary Stars: Application to Mass Transfer

2019 ◽  
Vol 50 (3) ◽  
pp. 507
Author(s):  
V.V. Sargsyan ◽  
H. Lenske ◽  
G.G. Adamian ◽  
N.V. Antonenko
Keyword(s):  
Mass Transfer ◽  
Binary Stars ◽  
Close Binary ◽  
Close Binary Stars

From dinuclear systems to close binary stars: Application to mass transfer

2018 ◽  
Vol 27 (07) ◽  
pp. 1850063 ◽  
Author(s):  
V. V. Sargsyan ◽  
H. Lenske ◽  
G. G. Adamian ◽  
N. V. Antonenko
Keyword(s):  
Mass Transfer ◽  
Binary Stars ◽  
Nuclear Physics ◽  
Total Mass ◽  
Close Binary ◽  
Stellar Systems ◽  
Star System ◽  
Mass Asymmetry ◽  
Symmetric Configuration ◽  
Close Binary Stars

Applying the microscopic nuclear physics ideas to macroscopic stellar systems, we study the evolution of the compact di-stars in mass asymmetry (transfer) coordinate. Depending on the internal structure of constituent stars, the initial mass asymmetry, total mass, and orbital angular momentum, the close di-star system can either exist in symmetric configuration or fuse into mono-star. The limitations for the formation of stable symmetric binary stars are analyzed.

scholarly journals The evolution of close binary stars: conditions in the winds

1995 ◽  
Vol 163 ◽  
pp. 291-299
Author(s):  
J.P. de Greve
Keyword(s):  
Mass Transfer ◽  
Binary Stars ◽  
Internal State ◽  
Close Binary ◽  
Close Binaries ◽  
Close Binary Stars ◽  
Wind Characteristics ◽  
Wind Regimes

The influence of mass transfer in an OB-type binary on the colliding wind characteristics of the following phase of WR binary is examined. We look to the changes in composition and orbital characteristics. Special attention is given to the formation of WR+OB systems and the colliding wind characteristics. The mass-luminosity behaviour after mass transfer is examined. We discuss the influence of the internal state, the composition of the wind, and rotational effects on the mass gainer. Recent models of both single stars and close binaries allow us to derive the dependence of these characteristics on the initial masses of the components. From this, constraints for the wind regimes at the WR+OB stage result.

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