2005/10/16 by Oleg Kargaltsev, O. Kargaltsev, George G. Pavlov +2 · 2 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black-body radiation #Flux (metallurgy) #Galaxy #High-pressure geophysics and materials #Isotropy #Luminosity #Neutron star #Optics #Photon #Physics #Polar #Polar cap #Power law #Pulsar #Pulsars and Gravitational Waves Research #Radiation #Spectral index #Spectral line #X-ray pulsar #astro-ph
paper · pdf · doi:10.1086/497897
published as Astrophys.J.636:406-410,2005 · 5 pages, 8 figures, accepted to ApJ
arxiv created 2005/10/16 · openalex publication_date 2005/12/21 · arxiv updated 2014/10/13 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We detected a nearby ( d ≃ 360 pc), old (τ ≃ 5 Myr) pulsar B1133+16 with Chandra . The observed pulsar's flux is (0.8 ± 0.2) × 10 -14 ergs cm -2 s -1 in the 0.5-8 keV band. Because of the small number of counts detected, the spectrum can be described by various models. A power-law fit of the spectrum gives a photon index Γ ≈ 2.5 and an isotropic luminosity of 1.4 × 10 29 ergs s -1 in the 0.5-8 keV band, which is about 1.6 × 10 -3 of the spin-down power . The spectrum can also be fitted by a blackbody model with a temperature of ≈2.8 MK and a projected emitting area of ~500 m 2 , possibly a hot polar cap. The X-ray properties of PSR B1133+16 are similar to those of other old pulsars observed in X-rays, particularly the drifting pulsar B0943+10.