<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Ho, Wynn C. G.</style></author><author><style face="normal" font="default" size="100%">Kuiper, Lucien</style></author><author><style face="normal" font="default" size="100%">Espinoza, Cristóbal M.</style></author><author><style face="normal" font="default" size="100%">Guillot, Sebastien</style></author><author><style face="normal" font="default" size="100%">Ray, Paul S.</style></author><author><style face="normal" font="default" size="100%">Smith, D. A.</style></author><author><style face="normal" font="default" size="100%">Bogdanov, Slavko</style></author><author><style face="normal" font="default" size="100%">Antonopoulou, Danai</style></author><author><style face="normal" font="default" size="100%">Arzoumanian, Zaven</style></author><author><style face="normal" font="default" size="100%">Bejger, Michał</style></author><author><style face="normal" font="default" size="100%">Enoto, Teruaki</style></author><author><style face="normal" font="default" size="100%">Esposito, Paolo</style></author><author><style face="normal" font="default" size="100%">Harding, Alice K.</style></author><author><style face="normal" font="default" size="100%">Haskell, Brynmor</style></author><author><style face="normal" font="default" size="100%">Lewandowska, Natalia</style></author><author><style face="normal" font="default" size="100%">Maitra, Chandreyee</style></author><author><style face="normal" font="default" size="100%">Vasilopoulos, Georgios</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910</style></title><short-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></short-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">1108</style></keyword><keyword><style  face="normal" font="default" size="100%">1306</style></keyword><keyword><style  face="normal" font="default" size="100%">1408</style></keyword><keyword><style  face="normal" font="default" size="100%">1822</style></keyword><keyword><style  face="normal" font="default" size="100%">464</style></keyword><keyword><style  face="normal" font="default" size="100%">Astrophysics - High Energy Astrophysical Phenomena</style></keyword><keyword><style  face="normal" font="default" size="100%">Astrophysics - Solar and Stellar Astrophysics</style></keyword><keyword><style  face="normal" font="default" size="100%">Ephemerides</style></keyword><keyword><style  face="normal" font="default" size="100%">Neutron stars</style></keyword><keyword><style  face="normal" font="default" size="100%">Pulsars</style></keyword><keyword><style  face="normal" font="default" size="100%">Rotation powered pulsars</style></keyword><keyword><style  face="normal" font="default" size="100%">X-ray sources</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2022</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2022/11/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2022ApJ...939....7H</style></url></web-urls></urls><publisher><style face="normal" font="default" size="100%">IOP</style></publisher><volume><style face="normal" font="default" size="100%">939</style></volume><pages><style face="normal" font="default" size="100%">7</style></pages><isbn><style face="normal" font="default" size="100%">0004-637X</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">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 $\dot{\nu }=(-6.2324\pm 0.0001)\times {10}^{-11}\,\mathrm{Hz}\,{{\rm{s}}}^{-1}$ but also for the first time the second time derivative of its spin rate $\ddot{\nu }=(4.2\pm 0.2)\times {10}^{-21}\,\mathrm{Hz}\,{{\rm{s}}}^{-2}$ . For the fastest and most energetic young pulsar, PSR J0537-6910 (with a 16 ms spin period), we detect four more glitches, for a total of 15 glitches over 4.5 yr 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 yr model to 4.4 yr, and for PSR J1849-0001, we extend the baseline from 1.5 to 4.7 yr. 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.</style></abstract></record></records></xml>