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Peering into the Dark Side: Magnesium Lines Establish a Massive Neutron Star in PSR J2215+5135

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dc.creatorLinares, Mauricio
dc.creatorShahbaz, Tspa
dc.creatorCasares, Jspa
dc.date.accessioned2020-08-19T14:40:04Z
dc.date.available2020-08-19T14:40:04Z
dc.date.created2018-05-23spa
dc.description.abstractNew millisecond pulsars (MSPs) in compact binaries provide a good opportunity to search for the most massive neutron stars. Their main-sequence companion stars are often strongly irradiated by the pulsar, displacing the effective center of light from their barycenter and making mass measurements uncertain. We present a series of optical spectroscopic and photometric observations of PSR J2215+5135, a “redback” binary MSP in a 4.14 hr orbit, and measure a drastic temperature contrast between the dark/cold (TN = 5660- + 380 260 K) and bright/hot (TD = 8080- + 280 470 K) sides of the companion star. We find that the radial velocities depend systematically on the atmospheric absorption lines used to measure them. Namely, the semi-amplitude of the radial velocity curve (RVC) of J2215 measured with magnesium triplet lines is systematically higher than that measured with hydrogen Balmer lines, by 10%. We interpret this as a consequence of strong irradiation, whereby metallic lines dominate the dark side of the companion (which moves faster) and Balmer lines trace its bright (slower) side. Further, using a physical model of an irradiated star to fit simultaneously the two-species RVCs and the three-band light curves, we find a center-of-mass velocity of K2 = 412.3 ± 5.0 km s?1 and an orbital inclination i = 63°.9- + 2.7 2.4. Our model is able to reproduce the observed fluxes and velocities without invoking irradiation by an extended source. We measure masses of M1 = 2.27- + 0.15 0.17 Me and M2 = 0.33- + 0.02 0.03 Me for the neutron star and the companion star, respectively. If confirmed, such a massive pulsar would rule out some of the proposed equations of state for the neutron star interior.eng
dc.format.mimetypeapplication/pdf
dc.identifier.doihttps://doi.org/10.3847/1538-4357/aabde6
dc.identifier.issnISSN: 0004-637X
dc.identifier.issnEISSN: 1538-4357
dc.identifier.urihttps://repository.urosario.edu.co/handle/10336/26702
dc.language.isoengspa
dc.publisherUniversity of Chicagospa
dc.relation.citationEndPage54
dc.relation.citationIssueNo. 1
dc.relation.citationStartPage1
dc.relation.citationTitleAstrophysical Journal
dc.relation.citationVolumeVol. 859
dc.relation.ispartofAstrophysical Journal, ISSN: 0004-637X; EISSN:1538-4357, Vol.859, No.1 (2018); pp. 1-54spa
dc.relation.urihttps://iopscience.iop.org/article/10.3847/1538-4357/aabde6spa
dc.rights.accesRightsinfo:eu-repo/semantics/openAccess
dc.rights.accesoAbierto (Texto Completo)spa
dc.sourceAstrophysical Journalspa
dc.source.instnameinstname:Universidad del Rosario
dc.source.reponamereponame:Repositorio Institucional EdocUR
dc.subject.keywordBinaries generalspa
dc.subject.keywordpulsars generalspa
dc.subject.keywordpulsars individualspa
dc.subject.keywordstars neutronspa
dc.subject.keywordStars variablesspa
dc.subject.keywordgeneral X-raysspa
dc.subject.keywordBinariesspa
dc.titlePeering into the Dark Side: Magnesium Lines Establish a Massive Neutron Star in PSR J2215+5135spa
dc.title.TranslatedTitlePeering into the Dark Side: Magnesium Lines Establish a Massive Neutron Star in PSR J2215 + 5135eng
dc.typearticleeng
dc.type.hasVersioninfo:eu-repo/semantics/publishedVersion
dc.type.spaArtículospa
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