Variability of the High Magnetic Field X-Ray Pulsar PSR J1846-0258 Associated with the Supernova Remnant Kes 75 as Revealed by the Chandra X-Ray Observatory

Details Variability of the High Magnetic Field X-Ray Pulsar PSR J1846-0258 Associated with the Supernova Remnant Kes 75 as Revealed by the Chandra X-Ray Observatory Variability of the High Magnetic Field X-Ray Pulsar PSR J1846-0258 Associated with the Supernova Remnant Kes 75 as Revealed by the Chandra X-Ray Observatory

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...678l..43k&link_type=abstract

The Astrophysical Journal, Volume 678, Issue 1, pp. L43-L46.

Astronomy and Astrophysics

Astronomy

34

Stars: Pulsars: Individual: Alphanumeric: Psr J1846-0258, Ism: Supernova Remnants, X-Rays: General

Scientific paper

We present results from the archival Chandra observations of the 0.3 s X-ray pulsar PSR J1846-0258 associated with the supernova remnant (SNR) Kes 75. The pulsar has the highest spin-down luminosity (Ė = 8.3 × 1036 ergs s-1) among all the high magnetic field pulsars (HBPs) and has been classified as a Crab-like pulsar despite its magnetic field (5 × 10 13 G) being above the quantum critical field. It is the only HBP described by a nonthermal Crab-like spectrum, powering a bright pulsar wind nebula (PWN). Our spectroscopic study shows evidence of spectral softening (photon index Γ = 1.32+0.08-0.09 to 1.97+0.05-0.07) and temporal brightening [unabsorbed flux Funabs = (4.3 +/- 0.2) × 10-12 to 2.7+0.1-0.2 × 10-11 ergs cm-2 s-1] of the pulsar by ~6 times from 2000 to 2006. The 0.5-10 keV luminosity of the pulsar at the revised distance of 6 kpc has also increased from LX = (1.85 +/- 0.08) × 1034 to 1.16+0.03-0.07 × 1035 ergs s-1, and the X-ray efficiency increased from 0.2% +/- 0.01% to 1.4+0.04-0.08%. The observed X-ray brightening and softening of the pulsar suggests for the first time that this HBP is revealing itself as a magnetar.

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