Maximum mass, moment of inertia and compactness of relativistic stars
A number of recent works have highlighted that it is possible to express the properties of general-relativistic stellar equilibrium configurations in terms of functions that do not depend on the specific equation of state employed to describe matter at nuclear densities. These functions are normally...
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description | A number of recent works have highlighted that it is possible to express the properties of general-relativistic stellar equilibrium configurations in terms of functions that do not depend on the specific equation of state employed to describe matter at nuclear densities. These functions are normally referred to as "universal relations" and have been found to apply, within limits, both to static or stationary isolated stars, as well as to fully dynamical and merging binary systems. Further extending the idea that universal relations can be valid also away from stability, we show that a universal relation is exhibited also by equilibrium solutions that are not stable. In particular, the mass of rotating configurations on the turning-point line shows a universal behaviour when expressed in terms of the normalised Keplerian angular momentum. In turn, this allows us to compute the maximum mass allowed by uniform rotation, M_{max}, simply in terms of the maximum mass of the nonrotating configuration, M_{TOV}, finding that M_{max} ~ (1.203 +- 0.022) M_{TOV} for all the equations of state we have considered. We further show that a universal relation can be found between the dimensionless moment of inertia and the stellar compactness. Although this relation is not surprising as it involves two quantities that have been shown to exhibit universal behaviour with other stellar properties, our parameterisation represents a refinement over a similar relation by Lattimer and Schutz (2005), where a different normalisation was used, and could provide an accurate tool to constrain the equation of state of nuclear matter when measurements of the moment of inertia become available. |
doi_str_mv | 10.48550/arxiv.1601.06083 |
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These functions are normally referred to as "universal relations" and have been found to apply, within limits, both to static or stationary isolated stars, as well as to fully dynamical and merging binary systems. Further extending the idea that universal relations can be valid also away from stability, we show that a universal relation is exhibited also by equilibrium solutions that are not stable. In particular, the mass of rotating configurations on the turning-point line shows a universal behaviour when expressed in terms of the normalised Keplerian angular momentum. In turn, this allows us to compute the maximum mass allowed by uniform rotation, M_{max}, simply in terms of the maximum mass of the nonrotating configuration, M_{TOV}, finding that M_{max} ~ (1.203 +- 0.022) M_{TOV} for all the equations of state we have considered. We further show that a universal relation can be found between the dimensionless moment of inertia and the stellar compactness. Although this relation is not surprising as it involves two quantities that have been shown to exhibit universal behaviour with other stellar properties, our parameterisation represents a refinement over a similar relation by Lattimer and Schutz (2005), where a different normalisation was used, and could provide an accurate tool to constrain the equation of state of nuclear matter when measurements of the moment of inertia become available.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1601.06083</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Angular momentum ; Binary stars ; Configurations ; Equations of state ; Inertia ; Moments of inertia ; Nuclear matter ; Parameterization ; Physics - General Relativity and Quantum Cosmology ; Physics - High Energy Astrophysical Phenomena ; Relativism ; Relativistic effects</subject><ispartof>arXiv.org, 2016-04</ispartof><rights>2016. 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These functions are normally referred to as "universal relations" and have been found to apply, within limits, both to static or stationary isolated stars, as well as to fully dynamical and merging binary systems. Further extending the idea that universal relations can be valid also away from stability, we show that a universal relation is exhibited also by equilibrium solutions that are not stable. In particular, the mass of rotating configurations on the turning-point line shows a universal behaviour when expressed in terms of the normalised Keplerian angular momentum. In turn, this allows us to compute the maximum mass allowed by uniform rotation, M_{max}, simply in terms of the maximum mass of the nonrotating configuration, M_{TOV}, finding that M_{max} ~ (1.203 +- 0.022) M_{TOV} for all the equations of state we have considered. We further show that a universal relation can be found between the dimensionless moment of inertia and the stellar compactness. Although this relation is not surprising as it involves two quantities that have been shown to exhibit universal behaviour with other stellar properties, our parameterisation represents a refinement over a similar relation by Lattimer and Schutz (2005), where a different normalisation was used, and could provide an accurate tool to constrain the equation of state of nuclear matter when measurements of the moment of inertia become available.</description><subject>Angular momentum</subject><subject>Binary stars</subject><subject>Configurations</subject><subject>Equations of state</subject><subject>Inertia</subject><subject>Moments of inertia</subject><subject>Nuclear matter</subject><subject>Parameterization</subject><subject>Physics - General Relativity and Quantum Cosmology</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Relativism</subject><subject>Relativistic effects</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2016</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotj0tLAzEUhYMgWGp_gCsDbp16c5NM0qWU-oCKm-6HdOYGUpqZmqSl_nv7cHUW5-NwPsYeBEyV1RpeXDqGw1TUIKZQg5U3bIRSisoqxDs2yXkDAFgb1FqO2OLLHUPcRx5dzs88DpH6wgfPQ0-pBMdd3_F2iDvXlp5yPleJtq6EQ8gltDwXl_I9u_Vum2nyn2O2elus5h_V8vv9c_66rJxGXXVolPHWri1hZ5HIeCSvOhQoW43GCl-vZwKo9cpLkE51namNFkgKZpLkmD1eZy-OzS6F6NJvc3ZtLq4n4ulK7NLws6dcms2wT_3pU4NgrBTGgJZ_Af9WlQ</recordid><startdate>20160411</startdate><enddate>20160411</enddate><creator>Breu, Cosima</creator><creator>Rezzolla, Luciano</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20160411</creationdate><title>Maximum mass, moment of inertia and compactness of relativistic stars</title><author>Breu, Cosima ; Rezzolla, Luciano</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a525-d2747f88b8e2d82ee7f2ef4d2123c52781f6b910ecf4f303a4dd767512e4093e3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2016</creationdate><topic>Angular momentum</topic><topic>Binary stars</topic><topic>Configurations</topic><topic>Equations of state</topic><topic>Inertia</topic><topic>Moments of inertia</topic><topic>Nuclear matter</topic><topic>Parameterization</topic><topic>Physics - General Relativity and Quantum Cosmology</topic><topic>Physics - High Energy Astrophysical Phenomena</topic><topic>Relativism</topic><topic>Relativistic effects</topic><toplevel>online_resources</toplevel><creatorcontrib>Breu, Cosima</creatorcontrib><creatorcontrib>Rezzolla, Luciano</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni)</collection><collection>ProQuest Central</collection><collection>ProQuest Central Essentials</collection><collection>AUTh Library subscriptions: ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>ProQuest - Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Breu, Cosima</au><au>Rezzolla, Luciano</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Maximum mass, moment of inertia and compactness of relativistic stars</atitle><jtitle>arXiv.org</jtitle><date>2016-04-11</date><risdate>2016</risdate><eissn>2331-8422</eissn><abstract>A number of recent works have highlighted that it is possible to express the properties of general-relativistic stellar equilibrium configurations in terms of functions that do not depend on the specific equation of state employed to describe matter at nuclear densities. These functions are normally referred to as "universal relations" and have been found to apply, within limits, both to static or stationary isolated stars, as well as to fully dynamical and merging binary systems. Further extending the idea that universal relations can be valid also away from stability, we show that a universal relation is exhibited also by equilibrium solutions that are not stable. In particular, the mass of rotating configurations on the turning-point line shows a universal behaviour when expressed in terms of the normalised Keplerian angular momentum. In turn, this allows us to compute the maximum mass allowed by uniform rotation, M_{max}, simply in terms of the maximum mass of the nonrotating configuration, M_{TOV}, finding that M_{max} ~ (1.203 +- 0.022) M_{TOV} for all the equations of state we have considered. We further show that a universal relation can be found between the dimensionless moment of inertia and the stellar compactness. Although this relation is not surprising as it involves two quantities that have been shown to exhibit universal behaviour with other stellar properties, our parameterisation represents a refinement over a similar relation by Lattimer and Schutz (2005), where a different normalisation was used, and could provide an accurate tool to constrain the equation of state of nuclear matter when measurements of the moment of inertia become available.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1601.06083</doi><oa>free_for_read</oa></addata></record> |
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subjects | Angular momentum Binary stars Configurations Equations of state Inertia Moments of inertia Nuclear matter Parameterization Physics - General Relativity and Quantum Cosmology Physics - High Energy Astrophysical Phenomena Relativism Relativistic effects |
title | Maximum mass, moment of inertia and compactness of relativistic stars |
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