File Download
  Links for fulltext
     (May Require Subscription)
Supplementary

Article: The statistical properties of X-ray emission from galactic young pulsars

TitleThe statistical properties of X-ray emission from galactic young pulsars
Authors
KeywordsPulsars: General
Stars: Neutron
Stars: Statistics
X-Rays: Stars
Issue Date1999
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X
Citation
Astrophysical Journal, 1999, v. 526 n. 1 PART 1, p. 327-335 How to Cite?
AbstractWe study statistical properties of the Galactic population of X-ray pulsars with ages of less than 106 yr using the Monte Carlo method. Combining the initial magnetic field and spatial and velocity distributions of neutron stars at birth (which are obtained from radio pulsar statistical studies) with either the X-ray pulsar model proposed by Cheng & Zhang or the expected X-ray flux obtained by the empirical formula proposed by Becker & Trümper, we obtain the distance, period, period derivative, and X-ray energy flux distributions of those X-ray pulsars whose X-ray and radio fluxes are above the detectable threshold fluxes. Our simulated results indicate that (1) the distance, period, period derivative, and X-ray energy flux distributions of simulated X-ray pulsars in both models are consistent with those of the known X-ray pulsars observed by ROSAT if the minimum detectable X-ray energy flux is 2 × 10-14 ergs cm-2 s-1, and (2) the expected X-ray pulsar numbers in both models are different; the ratio of expected X-ray pulsars in our model to those in Becker & Trümper's model is about 0.6. Moreover, as the minimum detectable X-ray energy flux decreases, the simulated distributions from the two models obviously differ except in the distance distributions, and especially so for the simulated distributions of the period and period derivative. As the minimum detectable X-ray energy flux decreases, those X-ray pulsars with long periods and small period derivatives become detectable. The next generation of X-ray satellites, e.g., XMM, may differentiate our model from that of Becker & Trümper.
Persistent Identifierhttp://hdl.handle.net/10722/174786
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266
References

 

DC FieldValueLanguage
dc.contributor.authorZhang, Len_US
dc.contributor.authorCheng, KSen_US
dc.date.accessioned2012-11-26T08:47:25Z-
dc.date.available2012-11-26T08:47:25Z-
dc.date.issued1999en_US
dc.identifier.citationAstrophysical Journal, 1999, v. 526 n. 1 PART 1, p. 327-335en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/174786-
dc.description.abstractWe study statistical properties of the Galactic population of X-ray pulsars with ages of less than 106 yr using the Monte Carlo method. Combining the initial magnetic field and spatial and velocity distributions of neutron stars at birth (which are obtained from radio pulsar statistical studies) with either the X-ray pulsar model proposed by Cheng & Zhang or the expected X-ray flux obtained by the empirical formula proposed by Becker & Trümper, we obtain the distance, period, period derivative, and X-ray energy flux distributions of those X-ray pulsars whose X-ray and radio fluxes are above the detectable threshold fluxes. Our simulated results indicate that (1) the distance, period, period derivative, and X-ray energy flux distributions of simulated X-ray pulsars in both models are consistent with those of the known X-ray pulsars observed by ROSAT if the minimum detectable X-ray energy flux is 2 × 10-14 ergs cm-2 s-1, and (2) the expected X-ray pulsar numbers in both models are different; the ratio of expected X-ray pulsars in our model to those in Becker & Trümper's model is about 0.6. Moreover, as the minimum detectable X-ray energy flux decreases, the simulated distributions from the two models obviously differ except in the distance distributions, and especially so for the simulated distributions of the period and period derivative. As the minimum detectable X-ray energy flux decreases, those X-ray pulsars with long periods and small period derivatives become detectable. The next generation of X-ray satellites, e.g., XMM, may differentiate our model from that of Becker & Trümper.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637Xen_US
dc.relation.ispartofAstrophysical Journalen_US
dc.subjectPulsars: Generalen_US
dc.subjectStars: Neutronen_US
dc.subjectStars: Statisticsen_US
dc.subjectX-Rays: Starsen_US
dc.titleThe statistical properties of X-ray emission from galactic young pulsarsen_US
dc.typeArticleen_US
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_US
dc.identifier.authorityCheng, KS=rp00675en_US
dc.description.naturelink_to_OA_fulltexten_US
dc.identifier.doi10.1086/307965-
dc.identifier.scopuseid_2-s2.0-0033589603en_US
dc.identifier.hkuros241910-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0033589603&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume526en_US
dc.identifier.issue1 PART 1en_US
dc.identifier.spage327en_US
dc.identifier.epage335en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridZhang, L=38762428100en_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats