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  • 1
    Electronic Resource
    Electronic Resource
    Evolution of massive close binaries (1975)
    Springer
    Astrophysics and space science 35 (1975), S. 241-247 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract X-ray binaries such as Cen X-3, Cyg X-1, Vela X-1, 2U1700-37, SMC X-1, Cir X-1, with periods ranging from 2d.087 to 12d.28, are probably evolution products of massive binary systems. The massive primary starts losing mass after core hydrogen burning and undergoes a supernova explosion. The evolution of binary systems consisting of a 20M⊙ primary and secondaries of respectively 14, 10, 8 and 6M⊙ was computed from Main Sequence stage through the X-ray phase, until the second mass transfer phase. Estimates were performed for the evolution of a secondary of 4M⊙. It may be seen that some of these systems during their X-ray phase match the observed mass ratios and periods.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00636994
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  • 2
    Electronic Resource
    Electronic Resource
    Evolution of massive close binaries (1975)
    Springer
    Astrophysics and space science 36 (1975), S. 219-225 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The further evolution of a massive X-ray binary consisting of a compact object and an OB supergiant is outlined. The supergiant exceeds its critical Roche lobe and a second stage of mass transfer starts. The remnant of the mass losing star — a pure helium star — develops a collapsing iron core and finally undergoes a supernova explosion. If the compact companion is a black hole the system remains bound; if the compact companion is a neutron star the system is disrupted unless an extra kick allowing an asymmetric explosion is given. Computations were performed for the massive binary 22.5M ⊙+2M ⊙. The possible final evolutionary products are: (1) a black hole and a compact object, in a binary system, (2) two run-away pulsars, (3) a binary pulsar. As final parameters for the described system the eccentricity and period for the recently discovered binary pulsar 1913+16 may be found. An orbital inclination ofi=40° may be derived. The probability for the generation of binary pulsars is very low; in most cases the system is disrupted during the supernova explosion.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00681952
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  • 3
    Electronic Resource
    Electronic Resource
    Close binary systems before and after mass transfer. II.Semi-detached systems (1980)
    Springer
    Astrophysics and space science 72 (1980), S. 411-432 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Recent data on semi-detached systems are compared with general results of close binary computations to determine the origin of Algol-type systems (classical case A and case B results are considered). Both the conservative and the non-conservative mode of mass exchange are investigated. It is found that the assumption of considerable mass loss from the system gives satisfying agreement with the observations. It is also concluded that the calculation of an extensive homogeneous network of case A computations is needed.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00639147
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  • 4
    Electronic Resource
    Electronic Resource
    Close binary systems before and after mass transfer: A comparison of observations and theory (1980)
    Springer
    Astrophysics and space science 68 (1980), S. 433-457 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract From a search through the literature 174 close binaries with known absolute dimensions have been sampled. Distinction is made between systems before and after mass exchange. Mass, period and mass ratio distributions and relations of the group of ‘unevolved’ binaries (i.e., prior to mass exchange) are transformed into corresponding distributions and relations of evolved binaries. The transformations are based upon theM 1f=g(M 1f) relation derived from an extended set of published theoretical computations of the evolution of close binaries. From this relation the following characteristics of the system after mass exchange are computed:M 1f,M 2f (andq f),P f. Five different modes of mass transfer were applied for the computation of the values ofP f andM 2f. The variation of the period was calculated using the formalism given by Vanbeverenet al. (1979). The results are compared to the observations of binary systems after mass exchange, and are discussed together with an analysis of the effect of several selection effects present in the distributions. The main conclusion is that, during mass exchange in close binaries, more than 50% of the mass is lost to the system in the process of transfer, removing a large amount of angular momentum.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00639709
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  • 5
    Electronic Resource
    Electronic Resource
    The evolution of massive close binaries (1977)
    Springer
    Astrophysics and space science 50 (1977), S. 75-85 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The final state of the primaries of binary systems with initial massesM 1i=10M ⊙ to 15M ⊙ is derived from the mass of their C/O-cores. The possibility of a second stage of mass transfer towards the secondary is considered. It turns out that the critical mass for the bifurcation is about 14M ⊙: stars with larger masses in this range are the progenitors of neutron stars, while the lower mass stars are the ancestors of white dwarfs.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00648520
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  • 6
    Electronic Resource
    Electronic Resource
    The evolution of massive close binaries (1978)
    Springer
    Astrophysics and space science 53 (1978), S. 105-130 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The results of evolutionary computations for massive binary systems (initial masses of the primary ≳10M ⊙) with mass ratios between 0.3 and 0.8 are summarized and compared with observations in order to verify how far one can go with the conservative assumption of mass exchange. It is found that conservative mass exchange leads to acceptable first-order models of W-R and massive X-ray binaries. However, the comparison between this theory and observation reveals that for the observed systems (W-R and X-ray binaries) a preference exists for low intial mass ratios; moreover, the X-ray luminosities of the theoretical models are systematically too low, though this may be due to the adopted wind model. In addition, the influences of several parameters (distance between the components, chemical composition, primary mass, mass ratio and atmosphere) are examined. These parameters influence the remnant mass and any further evolution only marginally. Attention is also given to the effect on the system parameters of a supernova explosion of the remnant of the mass-losing component. For a large range of systems a disruption probability smaller than 25% is found.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00645908
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  • 7
    Electronic Resource
    Electronic Resource
    Bifurcation points in close binary evolution: Medium-mass binaries (1982)
    Springer
    Astrophysics and space science 84 (1982), S. 447-456 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The remaining core hydrogen burning lifetime after case B of mass transfer of the secondary (mass gaining) component in a medium mass close binary star is estimated, for mediummass binaries with primaries in the mass range 5M ⊙ to 9M ⊙. From the comparison of this quantity with the helium burning time-scale of the remnant primary a critical mass ratioq c is derived such that for larger values ofq, mass transfer from the secondary towards the primary starts before the latter has evolved into a white dwarf. Consequences for the advanced stages of medium mass binaries are discussed.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00651323
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  • 8
    Electronic Resource
    Electronic Resource
    Structure and evolution of large groups of Massive Close Binary systems (1982)
    Springer
    Astrophysics and space science 87 (1982), S. 357-375 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Using the definition of four important events in the evolution of Massive Close Binary systems, we define five observable evolutionary phases in the life of a Massive Close Binary system: OB+OB, WR+OB, C+OB, C+WR, and WR+WR. We define and compute a number of observable phenomena for large groups of Massive Close Binaries. For one burst of star formation, we compute the number of systems in different evolutionary phases, and the total mass loss as functions of the time. For continuous star formation, we determine the fraction of WR binary stars, occurring in different phases of massive close binary evolution, and a number of average quantities (mass, mass ratio) of WR binary systems. The results are compared with observations of WR binaries in the Galaxy and in Open Clusters.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00648930
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  • 9
    Electronic Resource
    Electronic Resource
    Semi-detached binaries: The origin and present status of TU Mon, SX Cas, and DM Per (1984)
    Springer
    Astrophysics and space science 99 (1984), S. 313-317 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract An attempt is made to trace back the possible progenitor systems of the Algol-type binaries TU Mon, SX Cas, and DM Per. The present characteristics are compared to the result of the evolution of 9M 0+5.4M 0. The position of the hot components in the HRD is discussed with regard to the theoretical models.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00650255
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  • 10
    Electronic Resource
    Electronic Resource
    The evolution of massive close binaries (1975)
    Springer
    Astrophysics and space science 38 (1975), S. 301-312 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The influence of tidal, interaction on the periods of massive X-ray binaries during the postsupernova evolution is investigated. It is assumed that after a certain time the orbit has become circular and synchronous. The tidal effects of subsequent evolutionary changes in the moment of inertia of the massive component are calculated. It is shown that, as is already suggested by Sparks and Stecher (1974), for small mass ratios and short binary periods a tidal instability may occur resulting in an accelerating inward spiral motion. Before the onset of the instability the tidal forces maintain a nearly synchronous orbit. Possibly the orbits of Cen X-3 and 3 U 1700-37 are already unstable at present.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00647129
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