Timing six energetic rotation-powered X-ray pulsars, including the fast-spinning young PSR J0058-7218 and Big Glitcher PSR J0537-6910
| Autor: | Ho, Wynn C. G., Kuiper, Lucien, Espinoza, Cristobal M., Guillot, Sebastien, Ray, Paul S., Smith, D. A., Bogdanov, Slavko, Antonopoulou, Danai, Arzoumanian, Zaven, Bejger, Michal, Enoto, Teruaki, Esposito, Paolo, Harding, Alice K., Haskell, Brynmor, Lewandowska, Natalia, Maitra, Chandreyee, Vasilopoulos, Georgios |
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| Rok vydání: | 2022 |
| Předmět: | |
| Zdroj: | Astrophys. J. 939, 7 (2022) |
| Druh dokumentu: | Working Paper |
| DOI: | 10.3847/1538-4357/ac8743 |
| Popis: | 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. Comment: 18 pages, 17 figures; accepted for publication in ApJ; very minor edits and no changes to numbers |
| Databáze: | arXiv |
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