The stability of quark matter

Keith A. Olive

doi:10.1016/0370-2693(82)90992-3

The stability of quark matter

Keith A. Olive

Physics and Astronomy (Twin Cities)

Research output: Contribution to journal › Article › peer-review

9 Scopus citations

Abstract

The possibility of quark matter existing in the interior of neutron stars is examined under a wide variety of conditions. The existence of a "quark star" relies only on its stability against gravitational collapse after the transition to quark matter occurs. It is found that for all choices of temperature and density, a star can not remain stable with a quark interior. In the context of model given, a maximum temperature of 30 MeV and a corresponding maximum mass of 2.8 M_⊗ is derived for neutron stars.

Original language	English (US)
Pages (from-to)	137-140
Number of pages	4
Journal	Physics Letters B
Volume	116
Issue number	2-3
DOIs	https://doi.org/10.1016/0370-2693(82)90992-3
State	Published - Oct 7 1982

Bibliographical note

Funding Information:
I would like to thank W. Press and S. Teukolsky for valuable discussions. This work was supported in part by a Smithsonian Astrophysical Observatory Fellowship.

Copyright:
Copyright 2014 Elsevier B.V., All rights reserved.

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10.1016/0370-2693(82)90992-3

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abstract = "The possibility of quark matter existing in the interior of neutron stars is examined under a wide variety of conditions. The existence of a {"}quark star{"} relies only on its stability against gravitational collapse after the transition to quark matter occurs. It is found that for all choices of temperature and density, a star can not remain stable with a quark interior. In the context of model given, a maximum temperature of 30 MeV and a corresponding maximum mass of 2.8 M⊗ is derived for neutron stars.",

author = "Olive, {Keith A.}",

note = "Funding Information: I would like to thank W. Press and S. Teukolsky for valuable discussions. This work was supported in part by a Smithsonian Astrophysical Observatory Fellowship. Copyright: Copyright 2014 Elsevier B.V., All rights reserved.",

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AU - Olive, Keith A.

N1 - Funding Information: I would like to thank W. Press and S. Teukolsky for valuable discussions. This work was supported in part by a Smithsonian Astrophysical Observatory Fellowship. Copyright: Copyright 2014 Elsevier B.V., All rights reserved.

PY - 1982/10/7

Y1 - 1982/10/7

N2 - The possibility of quark matter existing in the interior of neutron stars is examined under a wide variety of conditions. The existence of a "quark star" relies only on its stability against gravitational collapse after the transition to quark matter occurs. It is found that for all choices of temperature and density, a star can not remain stable with a quark interior. In the context of model given, a maximum temperature of 30 MeV and a corresponding maximum mass of 2.8 M⊗ is derived for neutron stars.

AB - The possibility of quark matter existing in the interior of neutron stars is examined under a wide variety of conditions. The existence of a "quark star" relies only on its stability against gravitational collapse after the transition to quark matter occurs. It is found that for all choices of temperature and density, a star can not remain stable with a quark interior. In the context of model given, a maximum temperature of 30 MeV and a corresponding maximum mass of 2.8 M⊗ is derived for neutron stars.

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JO - Physics Letters B

JF - Physics Letters B

IS - 2-3

ER -

The stability of quark matter

Abstract

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