The equation of state in nucleon and strange stars

Journal Article · Thu May 01 00:00:00 EDT 1997 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.54308· OSTI ID:664850

Prakash, M ^[1]

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1. Department of Physics and Astronomy, State University of New York at Stony Brook, Stony Brook, New York11794 (United States)

The equation of state (EOS) is an essential physical ingredient in simulations of gravitational collapse, supernovae, old and newly born neutron stars, and binary mergers of compact stars. In this talk, I will examine (1) the extent to which stringent constraints may be placed on the EOS by a comparison of calculations with the available data on some basic neutron star properties; and (2) some astrophysical consequences of the possible presence of strangeness, in the form of baryons, notably the {Lambda} and {Sigma}{sup {minus}}, or as a Bose condensate, such as a K{sup {minus}} meson condensate, or in the form of strange quarks. {copyright} {ital 1997 American Institute of Physics.}

• Research Organization: New York State University Research Foundation
• Sponsoring Organization: USDOE
• DOE Contract Number: FG02-88ER40388
• OSTI ID: 664850
• Report Number(s): CONF-970564-; ISSN 0094-243X; TRN: 98:010883
• Journal Information: AIP Conference Proceedings, Vol. 412, Issue 1; Conference: 6. conference on the intersections of particle and nuclear physics, Big Sky, MT (United States), 25 May - 2 Jun 1997; Other Information: PBD: May 1997
• Country of Publication: United States
• Language: English

Related Subjects

66 PHYSICS
STARS
STRANGENESS
EQUATIONS OF STATE
SUPERNOVAE
NEUTRON STARS
LAMBDA PARTICLES
SIGMA MINUS PARTICLES
MASS