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  • 1
    Electronic Resource
    Electronic Resource
    The early evolution of the sun
    Amsterdam : Elsevier
    Icarus 1 (1962), S. 422-441 
    Details
    ISSN: 0019-1035
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1016/0019-1035(62)90045-3
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  • 2
    Electronic Resource
    Electronic Resource
    Main sequence for rotating stars of intermediate mass (1986)
    Springer
    Astrophysics and space science 126 (1986), S. 29-50 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We have investigated the evolutionary behaviour of intermediate mass (2, 3, 4, 5, and 7M ⊙) Population I stars, assuming two different rates of rotation at the threshold of stability. In the first part of the study, stars are assumed to start with a critical rotation (fast rotation model) and to progress to the point of rotational instability. The stars evolve by losing mass and become rotationally unstable before they reach the zero-age Main Sequence. It is argued that multiple star systems might be formed through the evolution of rapidly rotating stars. An expression for the rotational mass loss rate is derived as a function of the physical parameters of stars. In the second part of the study, stars are assumed to rotate at a rate below the critical value (slow rotation model). The evolution of slowly rotating stars is followed as far as zero-age Main Sequence on the theoretical Hertzsprung-Russell diagram and compared with that of normal stars. The evolutionary paths are found to be more or less similar to those of normal stars; but their positions on the Main Sequence are characterized by effective temperatures and luminosities lower than those of normal stars. The zero-age Main-Sequence times of these stars are longer than those of normal stars. The rotational rates obtained for the zero-age Main Sequence are in good agreement with observed values.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00644173
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  • 3
    Electronic Resource
    Electronic Resource
    The evolutionary behaviour of population III intermediate mass stars (1985)
    Springer
    Astrophysics and space science 117 (1985), S. 95-109 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Assuming the Big-Bang nucleosynthesis was responsible for the formation of helium, the evolution of first-generation intermediate-mass stars of 5, 7, and 9M ⊙ with no metals have been studied from the threshold of stability through the stage of helium exhaustion in the cores of the stars. Hydrogen Main-Sequence positions are marked at effective temperatures higher than those of normal stars. The evolutionary tracks during the hydrogen burning phase start to be similar to those of normal stars when the CN-cycle reactions, which are controlled by the triple-alpha reactions, become operative for hydrogen depletion. Helium Main Sequence of Population III stars of intermediate mass occurs at the high effective temperature region of the H-R diagram and stars stay as blue stars until the end of the core helium exhaustion phase. The total time elapsed is in the range of 3×107 and 108yr. The stars with the initial masses of 5, 7, and 9M ⊙ developed a moderately electron degenerate complete hydrogen-exhausted region with masses of 0.77, 1.06, and 1.42M ⊙, respectively, in which the most abundant element is carbon.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00660914
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  • 4
    Electronic Resource
    Electronic Resource
    Pregalactic-primordial low-mass stars (1987)
    Springer
    Astrophysics and space science 136 (1987), S. 83-90 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The Main-Sequence positions as well as the evolutionary behavior of Population III stars up to an evolution age of 2×1010 yr, taking this time as the age of the Universe, have been investigated in the mass range 0.2 and 0.8M ⊙. While Population III stars with masses greater than 0.3M ⊙ develop a radiative core during the approach to the Main Sequence, stars with masses smaller than 0.3M ⊙ reach the Main Sequence as a wholly convective stars. Population III stars with masses greater than 0.5M ⊙ show a brightening of at most 2.2 in bolometric magnitude when the evolution is terminated as compared to the value which corresponds to zero-age Main Sequence. The positions of stars with masses smaller than 0.5M ⊙ remain almost the same in the H-R diagram. If Population III stars have formed over a range of redshifts, 6〈Z〈1500, the original starlight of low-mass Population III stars could now be the part of infrared and/or microwave background spectrum between 7 and 1400 μm.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00661255
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  • 5
    Electronic Resource
    Electronic Resource
    Age determination of the open cluster NGC 2287 (M41) (1988)
    Springer
    Astrophysics and space science 147 (1988), S. 137-143 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We have estimated the age of the open cluster NGC 2287 (M41) by taking into account the rotation of the member stars. TheUBV photoelectric measurement values were taken from Eggen (1974). Besides the Main-Sequence stars this cluster has seven red giants, all of them above the turn-off point. Having obtained the theoretical Hertzsprung-Russell diagram from observed colour-magnitude diagram, we have discussed two methods, given in the literature, to estimate the age of the cluster under consideration. The first method we have followed is to determine the turn-off point on the cluster Main-Sequence. The other is fitting the position of the red giants with the evolutionary tracks of rotating stars with different masses on the Hertzsprung-Russell diagram. We have estimated the cluster age based on the turn-off point as 3.10×107 yr. From the fitting of the evolutionary tracks of rotating stars to the cluster Hertzsprung-Russell diagram, we infer that the age of the cluster is about 8.00×107 yr.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00656613
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  • 6
    Electronic Resource
    Electronic Resource
    A computation of the equation of state for a Fermi gas (1992)
    Springer
    Astrophysics and space science 190 (1992), S. 233-242 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Calculation of equation of state in stellar interiors becomes difficult as contained gas deviates from perfect gas. We present a method for the calculation of electron pressure in terms of density and temperature in the presence of degeneracy. The method is applicable forT〈109 K, and requires complete ionization.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00644850
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  • 7
    Electronic Resource
    Electronic Resource
    Convection zone of white-dwarf stars (1992)
    Springer
    Astrophysics and space science 187 (1992), S. 27-36 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The boundary convection zones of hot helium white-dwarf stars (WDSs) in the range 17000 K≤T e≤30000 K are studied. Recently, an anisotropic mixing-length theory (AMLT) which determines the mixing-length parameter locally is applied for the convection zones calculation. Comparing with the calculations by using the (MLT), it is found that maximum velocity decreases appreciably, and the other boundary conditions are affected.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00642685
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  • 8
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    Physical constraints determine the logic of bacterial promoter architectures (2014)
    Oxford University Press
    Details
    Publication Date: 2014-04-15
    Description: Site-specific transcription factors (TFs) bind to their target sites on the DNA, where they regulate the rate at which genes are transcribed. Bacterial TFs undergo facilitated diffusion (a combination of 3D diffusion around and 1D random walk on the DNA) when searching for their target sites. Using computer simulations of this search process, we show that the organization of the binding sites, in conjunction with TF copy number and binding site affinity, plays an important role in determining not only the steady state of promoter occupancy, but also the order at which TFs bind. These effects can be captured by facilitated diffusion-based models, but not by standard thermodynamics. We show that the spacing of binding sites encodes complex logic, which can be derived from combinations of three basic building blocks: switches, barriers and clusters, whose response alone and in higher orders of organization we characterize in detail. Effective promoter organizations are commonly found in the E. coli genome and are highly conserved between strains. This will allow studies of gene regulation at a previously unprecedented level of detail, where our framework can create testable hypothesis of promoter logic.
    Print ISSN: 0305-1048
    Electronic ISSN: 1362-4962
    Topics: Biology
    Published by Oxford University Press
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  • 9
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    Age determination of the open cluster NGC 2287 (M41) (1988)
    Springer
    Details
    Publication Date: 1988-01-01
    Print ISSN: 0004-640X
    Electronic ISSN: 1572-946X
    Topics: Physics
    Published by Springer
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  • 10
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    Main sequence for rotating stars of intermediate mass (1986)
    Springer
    Details
    Publication Date: 1986-01-01
    Print ISSN: 0004-640X
    Electronic ISSN: 1572-946X
    Topics: Physics
    Published by Springer
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