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  • 1
    Electronic Resource
    Electronic Resource
    Circular dichroism study of the interaction between T4 gene 32 protein and polynucleotides (1978)
    s.l. : American Chemical Society
    Biochemistry 17 (1978), S. 887-893 
    Details
    ISSN: 1520-4995
    Source: ACS Legacy Archives
    Topics: Biology , Chemistry and Pharmacology
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1021/bi00598a022
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  • 2
    Electronic Resource
    Electronic Resource
    Circular dichroism studies of the interaction of a limited hydrolysate of T4 gene 32 protein with T4 DNA and poly[d(A-T)].poly[d(A-T)] (1978)
    s.l. : American Chemical Society
    Biochemistry 17 (1978), S. 893-898 
    Details
    ISSN: 1520-4995
    Source: ACS Legacy Archives
    Topics: Biology , Chemistry and Pharmacology
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1021/bi00598a023
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  • 3
    Electronic Resource
    Electronic Resource
    Interspecific interaction: The analysis of complex structures in carnivorous zooplankton populations (1977)
    Springer
    Helgoland marine research 30 (1977), S. 83-91 
    Details
    ISSN: 1438-3888
    Source: Springer Online Journal Archives 1860-2000
    Topics: Biology
    Notes: Abstract Linear unidirectional dependence of one population upon another is rather atypical among zooplankton species, as carnivory is not only characteristic of high trophic levels but also part of omnivory in many species of copepods. The feeding on its predatorjuveniles may be important for the survival of a copepod population, more in regard to the impact on the predator than to the nutritional benefit obtained. Such complex interrelationships are important for predictive ecosystem models. Ctenophore-copepod interrelationships have been analysed in experiments, and the results produced have been used for constructing simulation models. Details of experimentation and of modelling are described and discussed.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF02207827
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  • 4
    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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  • 5
    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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  • 6
    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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  • 7
    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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  • 8
    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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  • 9
    Electronic Resource
    Electronic Resource
    Evolution of massive close binaries (1976)
    Springer
    Astrophysics and space science 43 (1976), S. 35-46 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The evolution of a binary system with components of 10M ⊙ and 8M ⊙ is computed through a case B of mass exchange. It is found that after the end of core helium burning, a second stage of mass transfer from the primary occurs. Carbon ignition is prohibited by the large neutrino losses in the degenerated core. The primary remnant, a 1.12M ⊙ star, ends as a white dwarf. A comparison with the 10M ⊙ single evolution is made.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00640553
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  • 10
    Electronic Resource
    Electronic Resource
    The Zeeman broadening of high n solar recombination lines (1975)
    Springer
    Solar physics 44 (1975), S. 371-382 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The Zeeman broadening of high n lines is derived. While in areas of the quiet Sun with field strengths of ≈1 G the upper boundary of the observable frequency region of recombination lines is defined by electron impact broadening, in active regions with field strengths ≳25 G the Zeeman broadening will shift this boundary to higher frequencies. The frequency region most favourable for observations is derived and the corresponding Doppler, electron impact and Zeeman broadening are discussed. The strengths of the recombination lines obtained in earlier calculations is reduced when one considers besides the Doppler broadening the electron impact and Zeeman broadening also. The frequency region favourable for observations is compared with the atmospheric transparency of the microwave region; it is found that observations require at least high altitude stations or space-based platforms. Details of using the Zeeman broadening of high n recombination lines for mapping (coronal) magnetic fields are given.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00153216
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