Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...395..240r&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 395, no. 1, p. 240-249.
Astronomy and Astrophysics
Astrophysics
88
Brunt-Vaisala Frequency, Charged Particles, Hot Stars, Neutron Stars, Stellar Oscillations, Gravitational Effects, Gravitational Waves, Stellar Cores
Scientific paper
Because a neutron star is born hot, its internal composition is close to chemical equilibrium. In the fluid core, this implies that the ratio of the number densities of charged particles (protons and electrons) to neutrons is an increasing function of the mass density. This composition gradient stably stratifies the matter giving rise to a Brunt-Vaisala frequency N of about 500/s. Consequently, a neutron star core provides a cavity that supports gravity modes (g-modes). These g-modes are distinct from those previously identified with the thermal stratification of the surface layers and the chemical stratification of the crust. We compute the lowest-order, quadrupolar, g-modes for cold, Newtonian, neutron star models with M/solar M = 0.581 and M/solar M = 1.405, and show that the crustal and core g-modes have similar periods. We also discuss damping mechanisms and estimate damping rates for the core g-modes. Particular attention is paid to damping due to the emission of gravitational radiation.
Goldreich Peter
Reisenegger Andreas
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