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| Format: | Preprint |
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2025
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| Online-Zugang: | https://arxiv.org/abs/2510.02233 |
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| _version_ | 1866911403172954112 |
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| author | Perez, K. I. Gotthelf, E. V. Halpern, J. P. |
| author_facet | Perez, K. I. Gotthelf, E. V. Halpern, J. P. |
| contents | We present a timing study of the three known central compact object (CCO) pulsars, isolated cooling neutron stars in supernova remnants, using Chandra, XMM-Newton and NICER observations spanning two decades. Relative to canonical young pulsars, CCOs are spinning down at a very slow rate $|\dot f| <10^{-15}$ s$^{-2}$, implying a surface dipole magnetic field strength $B_s < 10^{11}$ G that is too weak to account for their X-ray-emitting hot spots. Two CCO pulsars with sufficiently long monitoring, 1E 1207.4$-$5209 and PSR J0821$-$4300, are seen to deviate from steady spin-down; their timing residuals can be modeled by one or more glitches in $f$ and $\dot f$, or alternatively by extreme timing noise. For the third CCO pulsar, PSR J1852+0400, the sparse temporal coverage was insufficient to detect such effects. Glitch activity and timing noise in large samples of rotation-powered pulsars correlate best with $\dot f$, while the timing irregularities of the first two CCOs are extreme compared to pulsars of the same $\dot f$. Nevertheless, timing activity in CCOs may arise from properties that they share with other young but more energetic pulsars: high internal temperature, strong buried magnetic field and superfluid behavior. Alternatively, continuing low-level accretion of supernova debris is not ruled out as a source of timing noise in CCOs. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_02233 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Noisy Timing Behavior is a Feature of Central Compact Object Pulsars Perez, K. I. Gotthelf, E. V. Halpern, J. P. High Energy Astrophysical Phenomena We present a timing study of the three known central compact object (CCO) pulsars, isolated cooling neutron stars in supernova remnants, using Chandra, XMM-Newton and NICER observations spanning two decades. Relative to canonical young pulsars, CCOs are spinning down at a very slow rate $|\dot f| <10^{-15}$ s$^{-2}$, implying a surface dipole magnetic field strength $B_s < 10^{11}$ G that is too weak to account for their X-ray-emitting hot spots. Two CCO pulsars with sufficiently long monitoring, 1E 1207.4$-$5209 and PSR J0821$-$4300, are seen to deviate from steady spin-down; their timing residuals can be modeled by one or more glitches in $f$ and $\dot f$, or alternatively by extreme timing noise. For the third CCO pulsar, PSR J1852+0400, the sparse temporal coverage was insufficient to detect such effects. Glitch activity and timing noise in large samples of rotation-powered pulsars correlate best with $\dot f$, while the timing irregularities of the first two CCOs are extreme compared to pulsars of the same $\dot f$. Nevertheless, timing activity in CCOs may arise from properties that they share with other young but more energetic pulsars: high internal temperature, strong buried magnetic field and superfluid behavior. Alternatively, continuing low-level accretion of supernova debris is not ruled out as a source of timing noise in CCOs. |
| title | Noisy Timing Behavior is a Feature of Central Compact Object Pulsars |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2510.02233 |