Pinning down the superfluid and nuclear equation of state and measuring neutron star mass using pulsar glitches

Abstract

Pulsars are rotating neutron stars that are renowned for their timing precision, although glitches can interrupt the regular timing behavior when these stars are young. Glitches are thought to be caused by interactions between normal and superfluid matter in the star. We update our recent work on a new technique using pulsar glitch data to constrain superfluid and nuclear equation of state models, demonstrating how current and future astronomy telescopes can probe fundamental physics such as superfluidity near nuclear saturation and matter at supranuclear densities. Unlike traditional methods of measuring a star’s mass by its gravitational effect on another object, our technique relies on nuclear physics knowledge and therefore allows measurement of the mass of pulsars which are in isolation

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Identifiers

ORCID for Wynn C.G. Ho: orcid.org/0000-0002-6089-6836

ORCID for Nils Andersson: orcid.org/0000-0001-8550-3843

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