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Neutron star crustsWe calculate properties of neutron star matter at subnuclear densities using an improved nuclear Hamiltonian. Nuclei disappear and the matter becomes uniform at a density of about 0.6n(s), where n(s) of about 0.16/cu fm is the saturation density of nuclear matter. As a consequence, the mass of matter in the crusts of neutron stars is only about half as large as previously estimated. In about half of that crustal mass, nuclear matter occurs in shapes very different from the roughly spherical nuclei familiar at lower densities. The thinner crust and the unusual nuclear shape have important consequences for theories of the rotational and thermal evolution of neutron stars, especialy theories of glitches.
Document ID
19930042268
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Lorenz, C. P.
(NASA Headquarters Washington, DC United States)
Ravenhall, D. G.
(NASA Headquarters Washington, DC United States)
Pethick, C. J.
(Illinois Univ. Urbana, United States)
Date Acquired
August 16, 2013
Publication Date
January 25, 1993
Publication Information
Publication: Physical Review Letters
Volume: 70
Issue: 4
ISSN: 0031-9007
Subject Category
Astrophysics
Accession Number
93A26265
Funding Number(s)
CONTRACT_GRANT: NSF PHY-89-21025
CONTRACT_GRANT: NSF PHY-91-00283
CONTRACT_GRANT: NAGW-1583
Distribution Limits
Public
Copyright
Other

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