2010/07/31 by Margaret A. Livingstone, C.‐Y. Ng, C. -Y. Ng +5 · 93 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Flux (metallurgy) #Glitch #High-pressure geophysics and materials #Magnetar #Nebula #Neutron star #Noise (video) #Observatory #Physics #Pulsar #Pulsars and Gravitational Waves Research #Rotation (mathematics) #Stars #X-ray pulsar #astro-ph.HE
paper · pdf · doi:10.1088/0004-637x/730/2/66
published in The Astrophysical Journal 730(2), 66 (IOP Publishing) · 15 pages, 7 figures. ApJ, in press. Upper limit on blackbody component added, as well as additional discussion
arxiv created 2011/02/21 · openalex publication_date 2011/03/04 · arxiv updated 2015/05/19 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/08
The ∼800 year old pulsar J1846−0258 is a unique transition object between rotation-powered pulsars and magnetars: though behaving like a rotation-powered pulsar most of the time, in 2006 it exhibited a distinctly magnetar-like outburst accompanied by a large glitch. Here, we present X-ray timing observations taken with the Rossi X-ray Timing Explorer over a 2.2 year period after the X-ray outburst and glitch had recovered. We observe that the braking index of the pulsar, previously measured to be n = 2.65 ± 0.01, is now n = 2.16 ± 0.13, a decrease of 18% ± 5%. We also note a persistent increase in the timing noise relative to the pre-outburst level. Despite the timing changes, a 2009 Chandra X-ray Observatory observation shows that the X-ray flux and spectrum of the pulsar and its wind nebula are consistent with the quiescent levels observed in 2000.