THE DENSE MATTER EQUATION OF STATE FROM NEUTRON STAR RADIUS AND MASS MEASUREMENTS

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dc.contributor.authorOezel, Feryal
dc.contributor.authorPsaltis, Dimitrios
dc.contributor.authorGuever, Tolga
dc.contributor.authorBaym, Gordon
dc.contributor.authorHeinke, Craig
dc.contributor.authorGuillot, Sebastien
dc.date.accessioned2024-01-10T12:09:29Z
dc.date.available2024-01-10T12:09:29Z
dc.date.issued2016
dc.description.abstractWe present a comprehensive study of spectroscopic radius measurements of twelve neutron stars obtained during thermonuclear bursts or in quiescence. We incorporate, for the first time, a large number of systematic uncertainties in the measurement of the apparent angular sizes, Eddington fluxes, and distances, in the composition of the interstellar medium, and in the flux calibration of X-ray detectors. We also take into account the results of recent theoretical calculations of rotational effects on neutron star radii, of atmospheric effects on surface spectra, and of relativistic corrections to the Eddington critical flux. We employ Bayesian statistical frameworks to obtain neutron star radii from the spectroscopic measurements as well as to infer the equation of state from the radius measurements. Combining these with the results of experiments in the vicinity of nuclear saturation density and the observations of similar to 2 M-circle dot neutron stars, we place strong and quantitative constraints on the properties of the equation of state between approximate to 2-8 times the nuclear saturation density. We find that around M = 1.5 M-circle dot, the preferred equation of state predicts radii between 10.1 and 11.1 km. When interpreting the pressure constraints in the context of high density equations of state based on interacting nucleons, our results suggest a relatively weak contribution of the three-body interaction potential.
dc.description.funderNSF
dc.description.funderNASA ADAP grant
dc.description.funderIstanbul University
dc.description.funderNSERC
dc.description.funderAlexander von Humboldt Fellowship
dc.description.funderFONDECYT
dc.fechaingreso.objetodigital2024-05-30
dc.format.extent25 páginas
dc.fuente.origenWOS
dc.identifier.doi10.3847/0004-637X/820/1/28
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/0004-637X/820/1/28
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/76494
dc.identifier.wosidWOS:000372787000028
dc.information.autorucFísica;Guillot S;S/I;1015726
dc.issue.numero1
dc.language.isoen
dc.nota.accesoContenido parcial
dc.publisherIOP PUBLISHING LTD
dc.revistaASTROPHYSICAL JOURNAL
dc.rightsacceso restringido
dc.subjectdense matter
dc.subjectequation of state
dc.subjectstars: neutron
dc.subjectX-rays: binaries
dc.subjectX-rays: bursts
dc.subjectX-rays: stars
dc.subjectX-RAY-BURSTS
dc.subjectNEAR-INFRARED PROPERTIES
dc.subjectGLOBULAR-CLUSTERS
dc.subjectMODEL ATMOSPHERES
dc.subjectSPECTROSCOPIC MEASUREMENTS
dc.subjectSYSTEMATIC UNCERTAINTIES
dc.subjectCOMPTONIZED SPECTRA
dc.subjectTIMING-EXPLORER
dc.subjectKS 1731-260
dc.subject4U 1608-52
dc.titleTHE DENSE MATTER EQUATION OF STATE FROM NEUTRON STAR RADIUS AND MASS MEASUREMENTS
dc.typeartículo
dc.volumen820
sipa.codpersvinculados1015726
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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