Abstract Neutron stars in low mess binary systems (QPOs and other galactic bulge X-ray sources, millisecond pulsars, wide binary pulsars, globular cluster X-ray sources) pose a problem as to their origin. Since neither collapse of the evolved core of massive stars (the systems would not survive the attending explotions) nor capture of a previously formed neutron star (star densities too low and/or relative velocities too large in the corresponding regions) can explain those systems, direct collapse of a white dwarf into a neutron star has to be invoked. Rather than postulating evolutionary scenarios involving hypothetical (and in any case very rare) ONeMg white dwarfs, we show CO white dwarfs to be the most natural candidates to the progenitors of such neutron stars. Cool CO white dwarfs totally or partially solid can collapse upon mess accretion for a sizeable range of the relevant parameters (initial messes and temperatures, accretion rates). This conclusion is shown to be independent from the hypothesis made as to the chemical Composition of solid CO mixtures (although the range leading to colsapse depends upon it). The results of dynamical calculations of such collapses are briefly summarized.


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    Title :

    Cold C + O white dwarfs and neutron stars


    Contributors:
    Isern, J. (author) / Canal, R. (author) / Garcia, D. (author) / Garcia-Berro, E. (author) / Hernanz, M. (author) / Labay, J. (author)

    Published in:

    Advances in Space Research ; 8 , 2-3 ; 703-706


    Publication date :

    1988-01-01


    Size :

    4 pages




    Type of media :

    Article (Journal)


    Type of material :

    Electronic Resource


    Language :

    English




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