Timing six energetic rotation-powered X-ray pulsars, including the fast-spinning young PSR J0058-7218 and Big Glitcher PSR J0537-6910 - Archive ouverte HAL Accéder directement au contenu
Article Dans Une Revue Astrophys.J. Année : 2022

Timing six energetic rotation-powered X-ray pulsars, including the fast-spinning young PSR J0058-7218 and Big Glitcher PSR J0537-6910

Wynn C.G. Ho
  • Fonction : Auteur
Lucien Kuiper
  • Fonction : Auteur
Cristobal M. Espinoza
  • Fonction : Auteur
Paul S. Ray
  • Fonction : Auteur
Slavko Bogdanov
  • Fonction : Auteur
Danai Antonopoulou
  • Fonction : Auteur
Zaven Arzoumanian
  • Fonction : Auteur
Michal Bejger
Teruaki Enoto
  • Fonction : Auteur
Paolo Esposito
  • Fonction : Auteur
Alice K. Harding
  • Fonction : Auteur
Brynmor Haskell
  • Fonction : Auteur
Natalia Lewandowska
  • Fonction : Auteur
Chandreyee Maitra
  • Fonction : Auteur

Résumé

Measuring a pulsar's rotational evolution is crucial to understanding the nature of the pulsar. Here we provide updated timing models for the rotational evolution of six pulsars, five of which are rotation phase-connected using primarily NICER X-ray data. For the newly-discovered fast energetic young pulsar, PSR J0058-7218, we increase the baseline of its timing model from 1.4 days to 8 months and not only measure more precisely its spin-down rate nudot = (-6.2324+/-0.0001)x10^-11 Hz s^-1 but also for the first time the second time derivative of spin rate nuddot = (4.2+/-0.2)x10^-21 Hz s^-2. For the fastest and most energetic young pulsar, PSR J0537-6910 (with 16 ms spin period), we detect 4 more glitches, for a total of 15 glitches over 4.5 years of NICER monitoring, and show that its spin-down behavior continues to set this pulsar apart from all others, including a long-term braking index n = -1.234+/-0.009 and interglitch braking indices that asymptote to <~ 7 for long times after a glitch. For PSR J1101-6101, we measure a much more accurate spin-down rate that agrees with a previous value measured without phase-connection. For PSR J1412+7922 (also known as Calvera), we extend the baseline of its timing model from our previous 1-year model to 4.4 years, and for PSR J1849-0001, we extend the baseline from 1.5 years to 4.7 years. We also present a long-term timing model of the energetic pulsar, PSR J1813-1749, by fitting previous radio and X-ray spin frequencies from 2009-2019 and new ones measured here using 2018 NuSTAR and 2021 Chandra data.
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hal-03676099 , version 1 (11-04-2023)

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Wynn C.G. Ho, Lucien Kuiper, Cristobal M. Espinoza, Sebastien Guillot, Paul S. Ray, et al.. Timing six energetic rotation-powered X-ray pulsars, including the fast-spinning young PSR J0058-7218 and Big Glitcher PSR J0537-6910. Astrophys.J., 2022, 939 (1), pp.7. ⟨10.3847/1538-4357/ac8743⟩. ⟨hal-03676099⟩
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