Astrophysics and Space Science

, Volume 26, Issue 1, pp 25–46 | Cite as

Nucleosynthesis in supernova outbursts and the chemical composition of the envelopes of neutron stars

  • G. S. Bisnovatyi-Kogan
  • V. M. Chechetkin


The formation of chemical elements in the envelopes of neutron stars is considered at the densities ϱ=107 to 1013 g cm−3. It is shown, that the compression of cold and hot matter leads to different chemical compositions. The compression of cold matter is accompanied by a decrease of atomic weightA, up to ϱ≈3×1012 g cm−3. One may distinguish the following stages during the compression of hot matter: quasi-equilibrium, when there exists both nuclear equilibrium and kinetic equilibrium in β-processes; and limited equilibrium, when the total number of nuclei is constant.

It is shown that a nonequilibrium chemical composition may be formed in the envelopes of neutron stars where there is an excess of neutrons in the presence of superheavy nuclei.

The nuclear energy, stored in the neutron star envelope may be sufficient to support neutron star luminosity at a level of ∼ 1036 erg s−1 over a period of ∼ 105 yr. Possible applications to the problem of X-ray sources and pulsars are discussed.

The formation of the heavy nuclei in Supernovae explosions is considered briefly. Rough estimates are made for the differences in chemical composition of ejected matter during the explosions of stars of different masses and Supernovae of different types.


Neutron Star Chemical Element Nuclear Energy Heavy Nucleus Atomic weightA 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


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Copyright information

© D. Reidel Publishing Company 1974

Authors and Affiliations

  • G. S. Bisnovatyi-Kogan
    • 1
  • V. M. Chechetkin
    • 1
  1. 1.Institute of Applied MathematicsU.S.S.R. Academy of SciencesMoscowU.S.S.R.

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