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dc.contributor.authorRaithel, Carolyn A.*
dc.contributor.authorÖzel, Feryal*
dc.contributor.authorPsaltis, Dimitrios*
dc.date.accessioned2017-01-20T20:57:59Z
dc.date.available2017-01-20T20:57:59Z
dc.date.issued2016-10-26
dc.identifier.citationFROM NEUTRON STAR OBSERVABLES TO THE EQUATION OF STATE. I. AN OPTIMAL PARAMETRIZATION 2016, 831 (1):44 The Astrophysical Journalen
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/0004-637X/831/1/44
dc.identifier.urihttp://hdl.handle.net/10150/622054
dc.description.abstractThe increasing number and precision of measurements of neutron star masses, radii, and, in the near future, moments of inertia offer the possibility of precisely determining the neutron star equation of state (EOS). One way to facilitate the mapping of observables to the EOS is through a parametrization of the latter. We present here a generic method for optimizing the parametrization of any physically allowed EOS. We use mock EOS that incorporate physically diverse and extreme behavior to test how well our parametrization reproduces the global properties of the stars, by minimizing the errors in the observables of mass, radius, and the moment of inertia. We find that using piecewise polytropes and sampling the EOS with five fiducial densities between similar to 1-8 times the nuclear saturation density results in optimal errors for the smallest number of parameters. Specifically, it recreates the radii of the assumed EOS to within less than 0.5 km for the extreme mock EOS and to within less than 0.12 km for 95% of a sample of 42 proposed, physically motivated EOS. Such a parametrization is also able to reproduce the maximum mass to within 0.04 M-circle dot and the moment of inertia of a 1.338 M-circle dot. neutron star to within less than 10% for 95% of the proposed sample of EOS.
dc.description.sponsorshipNASA [NNX16AC56G]en
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/0004-637X/831/i=1/a=44?key=crossref.766f7d790f09e4c490ed9e8856cd1735en
dc.rights© 2016. The American Astronomical Society. All rights reserved.en
dc.subjectequation of stateen
dc.subjectstars: interiorsen
dc.subjectstars: neutronen
dc.titleFROM NEUTRON STAR OBSERVABLES TO THE EQUATION OF STATE. I. AN OPTIMAL PARAMETRIZATIONen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Dept Astronen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalThe Astrophysical Journalen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-05-18T09:54:49Z
html.description.abstractThe increasing number and precision of measurements of neutron star masses, radii, and, in the near future, moments of inertia offer the possibility of precisely determining the neutron star equation of state (EOS). One way to facilitate the mapping of observables to the EOS is through a parametrization of the latter. We present here a generic method for optimizing the parametrization of any physically allowed EOS. We use mock EOS that incorporate physically diverse and extreme behavior to test how well our parametrization reproduces the global properties of the stars, by minimizing the errors in the observables of mass, radius, and the moment of inertia. We find that using piecewise polytropes and sampling the EOS with five fiducial densities between similar to 1-8 times the nuclear saturation density results in optimal errors for the smallest number of parameters. Specifically, it recreates the radii of the assumed EOS to within less than 0.5 km for the extreme mock EOS and to within less than 0.12 km for 95% of a sample of 42 proposed, physically motivated EOS. Such a parametrization is also able to reproduce the maximum mass to within 0.04 M-circle dot and the moment of inertia of a 1.338 M-circle dot. neutron star to within less than 10% for 95% of the proposed sample of EOS.


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