Tomographic Separation of Composite Spectra. IV. The Physical Properties of the Massive Close Binary DH Cephei

1997 ◽  
Vol 483 (1) ◽  
pp. 439-448 ◽  
Author(s):  
Laura R. Penny ◽  
Douglas R. Gies ◽  
William G. Bagnuolo, Jr.
Keyword(s):  
Physical Properties ◽  
Close Binary ◽  
Composite Spectra ◽  
Massive Close Binary

Tomographic Separation of Composite Spectra. VI. The Physical Properties of the Massive Close Binary HD 152248

1999 ◽  
Vol 518 (1) ◽  
pp. 450-456 ◽  
Author(s):  
Laura R. Penny ◽  
Douglas R. Gies ◽  
William G. Bagnuolo, Jr.
Keyword(s):  
Physical Properties ◽  
Close Binary ◽  
Composite Spectra ◽  
Massive Close Binary

Tomographic Separation of Composite Spectra. X. The Massive Close Binary HD 101131

2002 ◽  
Vol 574 (2) ◽  
pp. 957-962 ◽  
Author(s):  
Douglas R. Gies ◽  
Laura R. Penny ◽  
Pavel Mayer ◽  
Horst Drechsel ◽  
Reinald Lorenz
Keyword(s):  
Close Binary ◽  
Composite Spectra ◽  
Massive Close Binary

Tomographic Separation of Composite Spectra. IX. The Massive Close Binary HD 115071

2002 ◽  
Vol 575 (2) ◽  
pp. 1050-1056 ◽  
Author(s):  
Laura R. Penny ◽  
Douglas R. Gies ◽  
John H. Wise ◽  
D. J. Stickland ◽  
C. Lloyd
Keyword(s):  
Close Binary ◽  
Composite Spectra ◽  
Massive Close Binary

Case a evolution of massive close binary systems

1987 ◽  
Vol 134 (1) ◽  
pp. 161-176 ◽  
Author(s):  
Masaomi Nakamura ◽  
Yasuhisa Nakamura
Keyword(s):  
Binary Systems ◽  
Close Binary ◽  
Close Binary Systems ◽  
Massive Close Binary

scholarly journals Apsidal motion in massive close binary systems – I. HD 165052, an extreme case?

2013 ◽  
Vol 433 (2) ◽  
pp. 1300-1311 ◽  
Author(s):  
G. Ferrero ◽  
R. Gamen ◽  
O. Benvenuto ◽  
E. Fernández-Lajús
Keyword(s):  
Binary Systems ◽  
Extreme Case ◽  
Close Binary ◽  
Apsidal Motion ◽  
Close Binary Systems ◽  
Massive Close Binary

scholarly journals The Massive Close Binary in the δ Ori A Triple System

2002 ◽  
Vol 187 ◽  
pp. 47-52
Author(s):  
James A. Harvin ◽  
Douglas R. Gies
Keyword(s):  
Cross Correlation ◽  
Short Wave ◽  
Close Binary ◽  
Full Description ◽  
High Dispersion ◽  
Orbital Elements ◽  
Primary Star ◽  
International Ultraviolet Explorer ◽  
Triple Star ◽  
Massive Close Binary

AbstractWe present an analysis of short-wave, high-dispersion ultraviolet spectra of the triple star δ Ori A from the International Ultraviolet Explorer Satellite’s (IUE) Final Archive. These spectra were cross-correlated against AE Aur to find the components’ radial velocities, which were then used to produce the system’s orbital elements. The long-period tertiary star in the δ Ori A system was not seen in the resulting cross-correlation functions (CCFs). The close binary’s eclipses allow the orbit’s inclination to be estimated by modeling of its Hipparcos light curve. The primary star appears to have a mass of 11.2 M⊙ and the secondary seems to have a mass of 5.6 M⊙, both of which are about 1/3 of the expected values for stars of their MK types. Although we expected the massive close binary in the δ Ori A system to be a pre-Roche lobe overflow (RLOF) system, these masses appear to require that it be a post-RLOF system. The full description of this work, including the tomographic separation of the spectra for the close binary’s components, appears in Harvin et al. (2002).

scholarly journals Two Types of Evolution of Massive Close Binary Systems

1976 ◽  
Vol 73 ◽  
pp. 27-34 ◽  
Author(s):  
C. De Loore ◽  
J. P. De Greve
Keyword(s):  
Mass Exchange ◽  
Binary Systems ◽  
Supernova Explosion ◽  
Close Binary ◽  
Helium Burning ◽  
Primary Star ◽  
Close Binary Systems ◽  
First Case ◽  
Initial Chemical Composition ◽  
Massive Close Binary

It is well known that the outcome of case B evolution of the primaries of massive close binary systems (M1 ≥ 9 M⊙) depends on the initial primary mass. The most massive primaries finally ignite carbon, form iron cores and presumably end in a supernova explosion, whereas the lighter ones presumably end as white dwarfs, without carbon ignition. This paper derives an estimate of the mass boundary separating these two kinds of evolution.As an example of the first case, the evolution of a 20 M⊙ + 14 M⊙ system was computed; after the mass exchange, the primary star (with M = 5.43 M⊙) evolves through the helium-burning (Wolf-Rayet) stage towards a supernova explosion; finally the system evolves into an X-ray binary (BWRX-evolution).As a representative for the second case the evolution of a 10 M⊙ + 8 M⊙ system was examined. After the first stage of mass exchange, the primary (with a mass of 1.66 M⊙) approaches the helium main sequence; during later phases of helium burning the radius increases again, and a second stage of mass transfer starts; after this the star (with a mass of 1.14 M⊙) again evolves towards the left in the Hertzsprung-Russell diagram and ends as a white dwarf (BSWD-evolution). A system of 15 M⊙ + 8 M⊙ is found to evolve very similar to the 20 M⊙ + 14 M⊙ system. The mass Mu, separating the two types of evolution, must therefore be situated between 10 and 15 solar masses. An initial chemical composition X = 0.70, Z = 0.03 was used for all systems.

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