Rossi X-Ray Timing Explorer Observation of PSR B0656+14

Details Rossi X-Ray Timing Explorer Observation of PSR B0656+14 Rossi X-Ray Timing Explorer Observation of PSR B0656+14

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...510..404c&link_type=abstract

The Astrophysical Journal, Volume 510, Issue 1, pp. 404-407.

Astronomy and Astrophysics

Astronomy

4

Stars: Pulsars: Individual: Alphanumeric: Psr B0656+14, X-Rays: Stars

Scientific paper

PSR B0656+14 was observed by the Rossi X-Ray Timing Explorer (RXTE) with the proportional counter array (PCA) and the high-energy X-ray timing experiment (HEXTE) for 160 ks during 1997 August 22-September 3. No pulsation was firmly found in the timing analysis, during which the contemporaneous radio ephemeris and various statistical tests were applied in searching for evidence of pulsation. A marginal detection of pulsation at a confidence level of 95.5% based on the H test was found with data in the whole HEXTE energy band. In the energy band of 2-10 keV the RXTE PCA upper limits are about 1 order of magnitude lower than that from ASCA GIS data. If the Compton Gamma Ray Observatory EGRET detection of this pulsar is real, considering the common trait that most EGRET-detected pulsars have a cooling spectrum in hard X-ray and gamma-ray energy bands, the estimated RXTE upper limits indicate a deviation (low-energy turnover) from a cooling spectrum starting from 20 keV or higher. This in turn suggests an outer magnetospheric synchrotron radiation origin for high-energy emissions from PSR B0656+14. The RXTE PCA upper limits also suggest that a reported power-law component based on ASCA SIS data in 1-10 keV fitted jointly with ROSAT data, if real, should be mainly unpulsed.

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