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Article: Hydrodynamic interaction between the be star and the pulsar in the TeV binary PSR B1259-63/LS 2883

TitleHydrodynamic interaction between the be star and the pulsar in the TeV binary PSR B1259-63/LS 2883
Authors
KeywordsBe
Gamma rays: Theory
Outflows
Stars: Emission-line
Stars: Individual (PSR B1259-63,LS 2883)
Stars: Winds
Issue Date2011
PublisherNihon Tenmon Gakkai. The Journal's web site is located at http://www.asj.or.jp/pasj/
Citation
Publications Of The Astronomical Society Of Japan, 2011, v. 63 n. 4, p. 893-901 How to Cite?
AbstractWe have been studying the interaction between the Be star and the pulsar in the TeV binary PSR B1259 63/LS 2883, using 3-D SPH simulations of the tidal and wind interactions in this Be-pulsar system. We first ran a simulation without pulsar wind nor Be wind, while taking into account only the gravitational effect of the pulsar on the Be disk. In this simulation, the gas particles are ejected at a constant rate from the equatorial surface of the Be star, which is tilted in a direction consistent with multi-waveband observations. We ran the simulation until the Be disk was fully developed and started to repeat a regular tidal interaction with the pulsar. Then, we turned on the pulsar wind and the Be wind. We ran two simulations with different wind mass-loss rates for the Be star, one for a B2V type and the other for a significantly earlier spectral type. Although the global shape of the interaction surface between the pulsar wind and the Be wind agrees with the analytical solution, the effect of the pulsar wind on the Be disk is profound. The pulsar wind strips off an outer part of the Be disk, truncating the disk at a radius significantly smaller than the pulsar orbit. Our results, therefore, rule out the idea that the pulsar passes through the Be disk around periastron, which has been assumed in previous studies. It also turns out that the location of the contact discontinuity can be significantly different between phases when the pulsar wind directly hits the Be disk and those when the pulsar wind collides with the Be wind. It is thus important to adequately take into account the circumstellar environment of the Be star, in order to construct a satisfactory model for this prototypical TeV binary. © 2011. Astronomical Society of Japan.
Persistent Identifierhttp://hdl.handle.net/10722/135363
ISSN
2015 Impact Factor: 1.961
2015 SCImago Journal Rankings: 0.804
References

 

DC FieldValueLanguage
dc.contributor.authorOkazaki, ATen_HK
dc.contributor.authorNagataki, Sen_HK
dc.contributor.authorNaito, Ten_HK
dc.contributor.authorKawachi, Aen_HK
dc.contributor.authorHayasaki, Ken_HK
dc.contributor.authorOwocki, SPen_HK
dc.contributor.authorTakata, Jen_HK
dc.date.accessioned2011-07-27T01:34:11Z-
dc.date.available2011-07-27T01:34:11Z-
dc.date.issued2011en_HK
dc.identifier.citationPublications Of The Astronomical Society Of Japan, 2011, v. 63 n. 4, p. 893-901en_HK
dc.identifier.issn0004-6264en_HK
dc.identifier.urihttp://hdl.handle.net/10722/135363-
dc.description.abstractWe have been studying the interaction between the Be star and the pulsar in the TeV binary PSR B1259 63/LS 2883, using 3-D SPH simulations of the tidal and wind interactions in this Be-pulsar system. We first ran a simulation without pulsar wind nor Be wind, while taking into account only the gravitational effect of the pulsar on the Be disk. In this simulation, the gas particles are ejected at a constant rate from the equatorial surface of the Be star, which is tilted in a direction consistent with multi-waveband observations. We ran the simulation until the Be disk was fully developed and started to repeat a regular tidal interaction with the pulsar. Then, we turned on the pulsar wind and the Be wind. We ran two simulations with different wind mass-loss rates for the Be star, one for a B2V type and the other for a significantly earlier spectral type. Although the global shape of the interaction surface between the pulsar wind and the Be wind agrees with the analytical solution, the effect of the pulsar wind on the Be disk is profound. The pulsar wind strips off an outer part of the Be disk, truncating the disk at a radius significantly smaller than the pulsar orbit. Our results, therefore, rule out the idea that the pulsar passes through the Be disk around periastron, which has been assumed in previous studies. It also turns out that the location of the contact discontinuity can be significantly different between phases when the pulsar wind directly hits the Be disk and those when the pulsar wind collides with the Be wind. It is thus important to adequately take into account the circumstellar environment of the Be star, in order to construct a satisfactory model for this prototypical TeV binary. © 2011. Astronomical Society of Japan.en_HK
dc.languageengen_US
dc.publisherNihon Tenmon Gakkai. The Journal's web site is located at http://www.asj.or.jp/pasj/en_HK
dc.relation.ispartofPublications of the Astronomical Society of Japanen_HK
dc.subjectBeen_HK
dc.subjectGamma rays: Theoryen_HK
dc.subjectOutflowsen_HK
dc.subjectStars: Emission-lineen_HK
dc.subjectStars: Individual (PSR B1259-63,LS 2883)en_HK
dc.subjectStars: Windsen_HK
dc.titleHydrodynamic interaction between the be star and the pulsar in the TeV binary PSR B1259-63/LS 2883en_HK
dc.typeArticleen_HK
dc.identifier.emailTakata, J: takata@hku.hken_HK
dc.identifier.authorityTakata, J=rp00786en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.scopuseid_2-s2.0-80051750077en_HK
dc.identifier.hkuros186459en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-80051750077&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume63en_HK
dc.identifier.issue4en_HK
dc.identifier.spage893en_HK
dc.identifier.epage901en_HK
dc.publisher.placeJapanen_HK
dc.identifier.scopusauthoridOkazaki, AT=7102544677en_HK
dc.identifier.scopusauthoridNagataki, S=7202476243en_HK
dc.identifier.scopusauthoridNaito, T=26024912200en_HK
dc.identifier.scopusauthoridKawachi, A=7004355934en_HK
dc.identifier.scopusauthoridHayasaki, K=25225640600en_HK
dc.identifier.scopusauthoridOwocki, SP=7003906613en_HK
dc.identifier.scopusauthoridTakata, J=22735157300en_HK

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