Formation enthalpy of monovacancies in neutron-star matter

Details Formation enthalpy of monovacancies in neutron-star matter Formation enthalpy of monovacancies in neutron-star matter

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999mnras.306..327j&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 306, Issue 2, pp. 327-332.

Astronomy and Astrophysics

Astronomy

14

Stars: Neutron, Pulsars: General

Scientific paper

Analysis of the monovacancy formation enthalpy in the solid phase of neutron-star matter has shown that neither the continuous neutron superfluid nor changes in nuclear properties are of significance. Its calculation is a well-defined problem involving Coulomb and electron energies. The thermal equilibrium concentrations of monovacancies obtained are too small to give superfluid-neutron-vortex pinning of the strength required to explain the sequence of large glitches observed in the Vela pulsar, but the monovacancy-vortex interaction, if attractive, could contribute to the recovery of the spin-down rate observed after a glitch.

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