File Download

There are no files associated with this item.

  Links for fulltext
     (May Require Subscription)
Supplementary

Article: THE unusual Ω̈ of the millisecond pulsar 1620-26: The consequence of a giant glitch?

TitleTHE unusual Ω̈ of the millisecond pulsar 1620-26: The consequence of a giant glitch?
Authors
KeywordsPulsars: Individual (Psr 1620-26)
Stars: Magnetic Fields
Issue Date1994
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 1994, v. 434 n. 2, p. 733-737 How to Cite?
AbstractWe suggest that the unusually large second derivative of angular velocity of PSR 1620-26 may result from a recent giant glitch which occurred more than 30 yr ago, instead of being caused by a second companion orbiting around the binary system of the pulsar. Our model parameters predict that either the core magnetic field of this pulsar is much stronger than its surface magnetic field if the internal torque is produced by the core superfluid, or Ω is actually larger than the present upper limit by a factor of several if the internal torque is produced by the crustal superfluid. The former case will indicate that the internal magnetic fields of both the canonical pulsars and millisecond pulsars are the same. We further suggest that PSR 1620-26 should be a soft X-ray source with L x ∼ 5 × 10 32 ergs -1 ergs and characteristic energy Eγ ∼ 200 eV.
Persistent Identifierhttp://hdl.handle.net/10722/174906
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_US
dc.contributor.authorChong, Nen_US
dc.contributor.authorLee, TMen_US
dc.date.accessioned2012-11-26T08:48:04Z-
dc.date.available2012-11-26T08:48:04Z-
dc.date.issued1994en_US
dc.identifier.citationAstrophysical Journal Letters, 1994, v. 434 n. 2, p. 733-737en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/174906-
dc.description.abstractWe suggest that the unusually large second derivative of angular velocity of PSR 1620-26 may result from a recent giant glitch which occurred more than 30 yr ago, instead of being caused by a second companion orbiting around the binary system of the pulsar. Our model parameters predict that either the core magnetic field of this pulsar is much stronger than its surface magnetic field if the internal torque is produced by the core superfluid, or Ω is actually larger than the present upper limit by a factor of several if the internal torque is produced by the crustal superfluid. The former case will indicate that the internal magnetic fields of both the canonical pulsars and millisecond pulsars are the same. We further suggest that PSR 1620-26 should be a soft X-ray source with L x ∼ 5 × 10 32 ergs -1 ergs and characteristic energy Eγ ∼ 200 eV.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectPulsars: Individual (Psr 1620-26)en_US
dc.subjectStars: Magnetic Fieldsen_US
dc.titleTHE unusual Ω̈ of the millisecond pulsar 1620-26: The consequence of a giant glitch?en_US
dc.typeArticleen_US
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_US
dc.identifier.authorityCheng, KS=rp00675en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.scopuseid_2-s2.0-12044250615en_US
dc.identifier.volume434en_US
dc.identifier.issue2en_US
dc.identifier.spage733en_US
dc.identifier.epage737en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US
dc.identifier.scopusauthoridChong, N=43960969800en_US
dc.identifier.scopusauthoridLee, TM=7501439535en_US

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats