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Structure of Quark Stars

Published online by Cambridge University Press:  20 March 2013

Fridolin Weber ,
Milva Orsaria ,
Hilario Rodrigues  and
Shu-Hua Yang
Fridolin Weber
Affiliation:
Department of Physics, San Diego State University, 5500 Campanile Drive, San Diego, California 92182, USA email: fweber@mail.sdsu.edu
Milva Orsaria
Affiliation:
CONICET, Rivadavia 1917, 1033 Buenos Aires; Gravitation, Astrophysics and Cosmology Group, Facultad de Ciencias Astronómicas y Geofisicas, Paseo del Bosque S/N (1900), Universidad Nacional de La Plata UNLP, La Plata, Argentina email: morsaria@fcaglp.fcaglp.unlp.edu.ar
Hilario Rodrigues
Affiliation:
Centro Federal de Educação Tecnológica do Rio de Janeiro, Av Maracanã 249, 20271-110, Rio de Janeiro, RJ, Brazil email: harg@cefet-rj.br
Shu-Hua Yang
Affiliation:
Institute of Astrophysics, Huazhong Normal University, Wuhan, 430079, P. R. China email: ysh@phy.ccnu.edu.cn
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Abstract

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This paper gives an brief overview of the structure of hypothetical strange quarks stars (quark stars, for short), which are made of absolutely stable 3-flavor strange quark matter. Such objects can be either bare or enveloped in thin nuclear crusts, which consist of heavy ions immersed in an electron gas. In contrast to neutron stars, the structure of quark stars is determined by two (rather than one) parameters, the central star density and the density at the base of the crust. If bare, quark stars possess ultra-high electric fields on the order of 1018 to 1019 V/cm. These features render the properties of quark stars more multifaceted than those of neutron stars and may allow one to observationally distinguish quark stars from neutron stars.

Keywords

neutron starsquark starspulsarsstrange quark matterequation of state
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S291: Neutron Stars and Pulsars: Challenges and Opportunities after 80 years , August 2012 , pp. 61 - 66
Copyright
Copyright © International Astronomical Union 2013

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