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Article: On the bimodal magnetic field distribution of binary pulsars

TitleOn the bimodal magnetic field distribution of binary pulsars
Authors
KeywordsDense matter
Magnetic fields
Pulsars: general
Stars: neutron
Issue Date1997
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 1997, v. 476 n. 1 PART II, p. L39-L42 How to Cite?
AbstractWe combine the idea of movement of magnetic flux tubes in the stellar interiors with the analysis of crustal physics of accreting neutron stars in low- and high-mass X-ray binaries to explain the bimodal magnetic field distribution of binary pulsars. We propose that this distribution may result from different crustal properties of neutron stars with different accretion rates and amounts of accreted matter. In addition, we may provide an explanation for why the magnetic field strengths of millisecond pulsars with low-mass companions saturate at ∼3 × 10 8 G when accreted mass exceeds ∼0.5 M ⊙. © 1997. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/43187
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_HK
dc.contributor.authorDai, ZGen_HK
dc.date.accessioned2007-03-23T04:40:57Z-
dc.date.available2007-03-23T04:40:57Z-
dc.date.issued1997en_HK
dc.identifier.citationAstrophysical Journal Letters, 1997, v. 476 n. 1 PART II, p. L39-L42en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/43187-
dc.description.abstractWe combine the idea of movement of magnetic flux tubes in the stellar interiors with the analysis of crustal physics of accreting neutron stars in low- and high-mass X-ray binaries to explain the bimodal magnetic field distribution of binary pulsars. We propose that this distribution may result from different crustal properties of neutron stars with different accretion rates and amounts of accreted matter. In addition, we may provide an explanation for why the magnetic field strengths of millisecond pulsars with low-mass companions saturate at ∼3 × 10 8 G when accreted mass exceeds ∼0.5 M ⊙. © 1997. The American Astronomical Society. All rights reserved.en_HK
dc.format.extent284236 bytes-
dc.format.extent12158 bytes-
dc.format.mimetypeapplication/pdf-
dc.format.mimetypetext/plain-
dc.languageengen_HK
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_HK
dc.relation.ispartofAstrophysical Journal Lettersen_HK
dc.rightsThe Astrophysical Journal. Copyright © University of Chicago Press.en_HK
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectDense matteren_HK
dc.subjectMagnetic fieldsen_HK
dc.subjectPulsars: generalen_HK
dc.subjectStars: neutronen_HK
dc.titleOn the bimodal magnetic field distribution of binary pulsarsen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=476&issue=pt 2&spage=L39&epage=L42&date=1997&atitle=On+the+Bimodal+Magnetic+Field+Distribution+of+Binary+Pulsarsen_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturepublished_or_final_versionen_HK
dc.identifier.doi10.1086/310486en_HK
dc.identifier.scopuseid_2-s2.0-21444455919en_HK
dc.identifier.hkuros21928-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-21444455919&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume476en_HK
dc.identifier.issue1 PART IIen_HK
dc.identifier.spageL39en_HK
dc.identifier.epageL42en_HK
dc.identifier.isiWOS:A1997WG53500010-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.scopusauthoridDai, ZG=7201387760en_HK

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