2020
DOI: 10.1093/mnras/staa2640
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Return of the Big Glitcher: NICER timing and glitches of PSR J0537−6910

Abstract: PSR J0537−6910, also known as the Big Glitcher, is the most prolific glitching pulsar known, and its spin-induced pulsations are only detectable in X-ray. We present results from analysis of 2.7 years of NICER timing observations, from 2017 August to 2020 April. We obtain a rotation phase-connected timing model for the entire timespan, which overlaps with the third observing run of LIGO/Virgo, thus enabling the most sensitive gravitational wave searches of this potentially strong gravitational wave-emitting pu… Show more

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Cited by 31 publications
(75 citation statements)
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“…The sign change simply maintains consistency with the model from Jaranowski et al (1998). The cause of such gravitational-wave emission is a deviation from axial symmetry, which can be written in terms of a dimensionless equatorial ellipticity ε, defined in terms of the star's principal moments of inertia 1 and 2 and from Ho et al (2020b) and the latter from Antonopoulou et al (2018). Errors in n ig are 1σ uncertainty.…”
Section: Model Of Gravitational-wave Emissionmentioning
confidence: 74%
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“…The sign change simply maintains consistency with the model from Jaranowski et al (1998). The cause of such gravitational-wave emission is a deviation from axial symmetry, which can be written in terms of a dimensionless equatorial ellipticity ε, defined in terms of the star's principal moments of inertia 1 and 2 and from Ho et al (2020b) and the latter from Antonopoulou et al (2018). Errors in n ig are 1σ uncertainty.…”
Section: Model Of Gravitational-wave Emissionmentioning
confidence: 74%
“…Its spin-down behavior appears to be driven by a process other than pure electromagnetic dipole radiation loss (at constant stellar magnetic field and moment of inertia). Specifically, its (long-term) braking indeẍ º =- n f f f 1.25 0.01 rot rot rot 2 , as measured over more than 20 yr (Ho et al 2020b), indicates an accelerating spin-down rate and significantly deviates from the measured values of most pulsars, n = 3, that imply dipole radiation (Shapiro & Teukolsky 1983).…”
Section: Introductionmentioning
confidence: 95%
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