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A new class of g-modes in neutron starsBecause 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.
Document ID
19930028523
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Reisenegger, Andreas (NASA Headquarters Washington, DC United States)
Goldreich, Peter (California Inst. of Technology Pasadena, United States)
Date Acquired
August 15, 2013
Publication Date
August 10, 1992
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 395
Issue: 1
ISSN: 0004-637X
Subject Category
ASTROPHYSICS
Funding Number(s)
CONTRACT_GRANT: NSF AST-89-13664
CONTRACT_GRANT: NAGW-1303
CONTRACT_GRANT: NAGW-2372
Distribution Limits
Public
Copyright
Other