Pinning down the superfluid and measuring masses using pulsar glitches

dc.contributor.authorHo, Wynn C. G.
dc.contributor.authorEspinoza, Cristobal M.
dc.contributor.authorAntonopoulou, Danai
dc.contributor.authorAndersson, Nils
dc.date.accessioned2025-01-23T21:33:57Z
dc.date.available2025-01-23T21:33:57Z
dc.date.issued2015
dc.description.abstractPulsars are known for their superb timing precision, although glitches can interrupt the regular timing behavior when the stars are young. These glitches are thought to be caused by interactions between normal and superfluid matter in the crust of the star. However, glitching pulsars such as Vela have been shown to require a superfluid reservoir that greatly exceeds that available in the crust. We examine a model in which glitches tap the superfluid in the core. We test a variety of theoretical superfluid models against the most recent glitch data and find that only one model can successfully explain up to 45 years of observational data. We develop a new technique for combining radio and x-ray data to measure pulsar masses, thereby demonstrating how current and future telescopes can probe fundamental physics such as superfluidity near nuclear saturation.
dc.fuente.origenWOS
dc.identifier.doi10.1126/sciadv.1500578
dc.identifier.issn2375-2548
dc.identifier.urihttps://doi.org/10.1126/sciadv.1500578
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/101525
dc.identifier.wosidWOS:000216598200009
dc.issue.numero9
dc.language.isoen
dc.revistaScience advances
dc.rightsacceso restringido
dc.titlePinning down the superfluid and measuring masses using pulsar glitches
dc.typeartículo
dc.volumen1
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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