On steady-state nuclear burning in accreting neutron stars

Ronald E Taam

doi:10.1007/BF00648773

On steady-state nuclear burning in accreting neutron stars

Ronald E Taam^*

^*Corresponding author for this work

Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

6 Scopus citations

Abstract

The properties of the hydrogen burning shell in the envelope of an accreting neutron star have been studied for a range of mass accretion rates, neutron star radii, and metal abundances of the accreted matter. It is found that the hydrogen burning shells lie at densities ranging from 10⁵-6×10⁶ gm cm^-3. For mass accretion rates in excess of M_c2 hydrogen and helium burn together. For M_c1≲M≲M_c2, the hydrogen burning shell is stabilized by the β limited CNO cycle. Implications of these results to the X-ray burst phenomena are briefly discussed.

Original language	English (US)
Pages (from-to)	257-265
Number of pages	9
Journal	Astrophysics and Space Science
Volume	77
Issue number	1
DOIs	https://doi.org/10.1007/BF00648773
State	Published - Jun 1 1981

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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abstract = "The properties of the hydrogen burning shell in the envelope of an accreting neutron star have been studied for a range of mass accretion rates, neutron star radii, and metal abundances of the accreted matter. It is found that the hydrogen burning shells lie at densities ranging from 105-6×106 gm cm-3. For mass accretion rates in excess of Mc2 hydrogen and helium burn together. For Mc1≲M≲Mc2, the hydrogen burning shell is stabilized by the β limited CNO cycle. Implications of these results to the X-ray burst phenomena are briefly discussed.",

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AB - The properties of the hydrogen burning shell in the envelope of an accreting neutron star have been studied for a range of mass accretion rates, neutron star radii, and metal abundances of the accreted matter. It is found that the hydrogen burning shells lie at densities ranging from 105-6×106 gm cm-3. For mass accretion rates in excess of Mc2 hydrogen and helium burn together. For Mc1≲M≲Mc2, the hydrogen burning shell is stabilized by the β limited CNO cycle. Implications of these results to the X-ray burst phenomena are briefly discussed.

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