期刊
ASTROPHYSICAL JOURNAL
卷 734, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/734/1/44
关键词
pulsars: individual (PSR J1718-3718); stars: neutron; X-rays: stars
资金
- NSERC
- CIFAR
- FQRNT
- Sloan Foundation
- Research Corporation
- Smithsonian Astrophysical Observatory award [GO9-0083A]
- Commonwealth of Australia
- NASA [NNX09AC84G]
- NASA [NNX09AC84G, 120557] Funding Source: Federal RePORTER
- Office Of Internatl Science &Engineering
- Office Of The Director [0968296] Funding Source: National Science Foundation
High-magnetic-field pulsars represent an important class of objects for studying the relationship between magnetars and radio pulsars. Here we report on four Chandra observations of the high-magnetic-field pulsar J1718-3718 (B = 7.4 x 10(13) G) taken in 2009 as well as a reanalysis of 2002 Chandra observations of the region. We also report an improved radio position for this pulsar based on ATCA observations. We detect X-ray pulsations at the pulsar's period in the 2009 data, with a pulsed fraction of 52% +/- 13% in the 0.8-2.0 keV band. We find that the X-ray pulse is aligned with the radio pulse. The data from 2002 and 2009 show consistent spectra and fluxes: a merged overall spectrum is well fit by a blackbody of temperature 186(-18)(+19) eV, slightly higher than predicted by standard cooling models; however, the best-fit neutron star atmosphere model is consistent with standard cooling. We find the bolometric luminosity L-bb(infinity) = 4(-2)(+5) x 10(32) erg s(-1) similar to 0.3 (E) over dot for a distance of 4.5 kpc. We compile measurements of the temperatures of all X-ray-detected high-B pulsars as well as those of low-B radio pulsars and find evidence for the former being hotter on average than the latter.
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