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.

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 Observational Evidence for Mass Exchange in Close Binary Systems

1977 ◽  
Vol 42 ◽  
pp. 371-382
Author(s):  
Horst Drechsel ◽  
Jürgen Rahe ◽  
Gudrun Wolfschmidt ◽  
Yoji Kondo ◽  
George E. McCluskey
Keyword(s):  
Northern Hemisphere ◽  
Mass Exchange ◽  
Binary Systems ◽  
Variable Stars ◽  
Observational Evidence ◽  
Close Binary ◽  
Wide Angle ◽  
Close Binary Systems ◽  
The Individual

In 1925 a photographic search for new variable stars was begun at the Remeis-Observatory in Bamberg. Initially the sky patrol covered only the northern hemisphere, but in 1964 it was also extended to the southern sky. At the individual observing stations, the sky is systematically photographed with several wide-angle patrol cameras which are attached to the same mounting, and which have f/6 Tessar lenses of 4-inch aperture. Each camera covers a 13-by-13 degree field. The plates are usually exposed for one hour and a photographic magnitude of 14m is reached.

scholarly journals A Review of Early-Type Close Binary Systems

1984 ◽  
Vol 80 ◽  
pp. 237-237
Author(s):  
K. C. Leung
Keyword(s):  
Mass Exchange ◽  
Binary Systems ◽  
Close Binary ◽  
Early Type ◽  
Close Binary Systems ◽  
Two Systems ◽  
V729 Cyg ◽  
Photometric Solution ◽  
Roche Model ◽  
Absolute Dimensions

AbstractThis is a review of close binary systems with very early spectral types (B, O, Of, and WR stars). We limit our selection to systems with Roche model photometric solution only. There are 10 contact systems known at present. Three of them (V701 Sco, BH Cen, and RZ Pyx) are located in the vicinity of the zero-age contact (ZC) according to a Spectral Type - Period diagram. Only the first two systems have absolute dimensions available. Both of these fall into the ZC zone in the logP - logm diagram and the logm - logR diagram. The system TU Mus was thought to be a ZC system is located in the evolved contact zone (EC) in the above diagrams. Both V701 Sco and BH Cen were thought to be having mass ratios about unity. With the much improved light curves of BH Cen and new analysis the mass ratio has been revised to 0.84! This result may favor Shu's model for early-type zero-age contact systems. The evolved systems might be undergone Case A mass exchange except for two systems (V729 Cyg and RY Set) which might be from Case B. The systems V367 Cyg was classified by Plavec as a W Ser system may be a evolved contact system.It is interesting to note that V729 Cyg (07f + Ofla), UW CMa(07f + O) and CQ Cep(WN7 + O) are all highly evolved contact systems. The Max II of UW CMa and CQ Cep are displaced to 0.78 and 0.80 phase, respectively. The displacement for V729 Cyg is not known due to poor coverage at this phase. The most distinct feature going from Of to Wolf-Rayet stars is the increasing domination of emission lines. It is suspected that this phaseshifts reflect the increasing activity of mass-flow in the common envelope.There are 8 semidetached systems with reliable absolute dimensions. It is believed that 6 of them are derived from Case A while the remaining 2 are from Case B mass exchange.

scholarly journals Late Stages of Close Binary Systems

1976 ◽  
Vol 73 ◽  
pp. 35-61 ◽  
Author(s):  
E. P. J. Van Den Heuvel
Keyword(s):  
Angular Momentum ◽  
Mass Exchange ◽  
Binary Systems ◽  
Main Sequence ◽  
Supernova Explosion ◽  
Compact Stars ◽  
Close Binary ◽  
Close Binaries ◽  
X Ray ◽  
Loss Of Mass

The expected final evolution of massive close binaries (CB) in case B is reviewed. Primary stars with masses ≳ 12–15 M⊙ are, after loosing most of their envelope by mass exchange, expected to explode as supernovae, leaving behind a neutron star or a black hole.Conservative close binary evolution (i.e. without a major loss of mass and angular momentum from the system during the first stage of mass transfer) is expected to occur if the initial mass ratio q0 = M20/M10 is ≳ 0.3. In this case the primary star will be the less massive component when it explodes, and the system is almost never disrupted by the explosion. The explosion is followed by a long-lasting quiet stage (106–107 yr) when the system consists of a massive main-sequence star and an inactive compact companion. After the secondary has left the main-sequence and becomes a blue supergiant with a strong stellar wind, the system becomes a massive X-ray binary for a short while (2–5 × 104 yr).The numbers of Wolf-Rayet binaries and massive X-ray binaries observed within 3 kpc of the Sun are in reasonable agreement with the numbers expected on the basis of conservative CB evolution, which implies that several thousands of massive main-sequence stars with a quiet compact companion should exist in the Galaxy. About a dozen of these systems must be present among the stars visible to the naked eye. During the second stage of mass exchange, large loss of mass and angular momentum from the system is expected, leading to a rapid shrinking of the orbit. The supernova explosion of the secondary will in most cases disrupt the system. If it remains bound, the final system will consist of two compact stars and may resemble the binary pulsar PSR 1913 + 16.In systems with q0 ≲ 0.2–0.3 large mass loss from the system is expected during the first stage of mass exchange. The exploding primary will then be more massive than its unevolved companion and the first supernova explosion disrupts the system in most cases. In the rare cases that it remains bound, the system will have a large runaway velocity and, after a very long (108–109 yr) inactive stage evolves into a low-mass X-ray binary, possibly resembling Her X-1.

Case a evolution of massive close binary systems

1987 ◽  
Vol 134 (2) ◽  
pp. 219-234 ◽  
Author(s):  
Masaomi Nakamura ◽  
Yasuhisa Nakamura
Keyword(s):  
Binary Systems ◽  
Close Binary ◽  
Close Binary Systems ◽  
Massive Close Binary
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