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Article: Modeling high-energy light curves of the PSRB1259-63/LS 2883 binary based on 3D SPH simulations

TitleModeling high-energy light curves of the PSRB1259-63/LS 2883 binary based on 3D SPH simulations
Authors
Keywordshydrodynamics
pulsars: individual (PSR B1259?63)
radiation mechanisms: non-thermal
stars: individual (LS 2883)
Issue Date2012
PublisherInstitute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/
Citation
Astrophysical Journal, 2012, v. 750 n. 1 How to Cite?
AbstractTemporal changes of X-ray to very high energy gamma-ray emissions from the pulsar-Be-star binary PSRB1259-63/LS 2883 are studied based on three-dimensional smoothed particle hydrodynamic simulations of pulsar wind interaction with Be-disk and wind. We focus on the periastron passage of the binary and calculate the variation of the synchrotron and inverse-Compton emissions using the simulated shock geometry and pressure distribution of the pulsar wind. The characteristic double-peaked X-ray light curve from observations is reproduced by our simulation under a dense Be-disk condition (base density ∼10 -9 g cm -3). We interpret the pre- and post-periastron peaks as being due to a significant increase in the conversion efficiency from pulsar spin-down power to the shock-accelerated particle energy at orbital phases when the pulsar crosses the disk before periastron passage, and when the pulsar wind creates a cavity in the disk gas after periastron passage, respectively. On the contrary, in the modelTeV light curve, which also shows a double-peak feature, the first peak appears around the periastron phase. The possible effects of cooling processes on theTeV light curve are briefly discussed. © 2012. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/146903
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266
ISI Accession Number ID
Funding AgencyGrant Number
Ministry of Education, Culture, Sports, Science and Technology (MEXT)23105709
Japan Society for the Promotion of Science (JSPS)19104006
23340069
23540271
Joint Usage/Research Center for Interdisciplinary Large-scale Information Infrastructures in Japan
MEXT of Japan
NASANNX11AC40G
iiC collaborative research program23105709
18104003
19047004
19740100
20540236
21105509
21540304
22340045
22540243
Hokkai-Gakuen Educational Foundation
Funding Information:

We express our appreciation to an anonymous referee for useful comments. J.T. thanks K. S. Cheng and R. E. Taam for useful discussions. S.N. is supported by Grant-in-Aid for Scientific Research on Innovative Areas No. 23105709 by Ministry of Education, Culture, Sports, Science and Technology (MEXT), Grant-in-Aid for Scientific Research (S) No. 19104006 and Scientific Research (B) No. 23340069 by Japan Society for the Promotion of Science (JSPS), Joint Usage/Research Center for Interdisciplinary Large-scale Information Infrastructures in Japan, and Grant-in-Aid for the Global COE Program "The Next Generation of Physics, Spun from Universality and Emergence" from MEXT of Japan. T.N. is supported by Grant-in-Aid for Scientific Research (C) No. 23540271 by Japan Society for the Promotion of Science (JSPS). S.P.O acknowledges partial support from grant NNX11AC40G from NASA's Astrophysics Theory Program. The computation was carried out on HITACHI SR16000 at Yukawa Institute for Theoretical Physics (YITP), Kyoto University, and on HITACHI SR11000 at the Information Initiative Center (iiC), Hokkaido University. In addition to the above grants, this work was partially supported by the iiC collaborative research program 2010-2011, the Grant-in-Aid for Scientific Research (18104003, 19047004, 19740100, 20540236, 21105509, 21540304, 22340045, 22540243, 23105709), and a research grant from Hokkai-Gakuen Educational Foundation.

References

 

DC FieldValueLanguage
dc.contributor.authorTakata, Jen_HK
dc.contributor.authorOkazaki, ATen_HK
dc.contributor.authorNagataki, Sen_HK
dc.contributor.authorNaito, Ten_HK
dc.contributor.authorKawachi, Aen_HK
dc.contributor.authorLee, SHen_HK
dc.contributor.authorMori, Men_HK
dc.contributor.authorHayasaki, Ken_HK
dc.contributor.authorYamaguchi, MSen_HK
dc.contributor.authorOwocki, SPen_HK
dc.date.accessioned2012-05-23T05:49:05Z-
dc.date.available2012-05-23T05:49:05Z-
dc.date.issued2012en_HK
dc.identifier.citationAstrophysical Journal, 2012, v. 750 n. 1en_HK
dc.identifier.issn0004-637Xen_HK
dc.identifier.urihttp://hdl.handle.net/10722/146903-
dc.description.abstractTemporal changes of X-ray to very high energy gamma-ray emissions from the pulsar-Be-star binary PSRB1259-63/LS 2883 are studied based on three-dimensional smoothed particle hydrodynamic simulations of pulsar wind interaction with Be-disk and wind. We focus on the periastron passage of the binary and calculate the variation of the synchrotron and inverse-Compton emissions using the simulated shock geometry and pressure distribution of the pulsar wind. The characteristic double-peaked X-ray light curve from observations is reproduced by our simulation under a dense Be-disk condition (base density ∼10 -9 g cm -3). We interpret the pre- and post-periastron peaks as being due to a significant increase in the conversion efficiency from pulsar spin-down power to the shock-accelerated particle energy at orbital phases when the pulsar crosses the disk before periastron passage, and when the pulsar wind creates a cavity in the disk gas after periastron passage, respectively. On the contrary, in the modelTeV light curve, which also shows a double-peak feature, the first peak appears around the periastron phase. The possible effects of cooling processes on theTeV light curve are briefly discussed. © 2012. The American Astronomical Society. All rights reserved.en_HK
dc.languageengen_US
dc.publisherInstitute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/en_HK
dc.relation.ispartofAstrophysical Journalen_HK
dc.rightsThe Astrophysical Journal. Copyright © Institute of Physics Publishing, Inc.-
dc.subjecthydrodynamicsen_HK
dc.subjectpulsars: individual (PSR B1259?63)en_HK
dc.subjectradiation mechanisms: non-thermalen_HK
dc.subjectstars: individual (LS 2883)en_HK
dc.titleModeling high-energy light curves of the PSRB1259-63/LS 2883 binary based on 3D SPH simulationsen_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.doi10.1088/0004-637X/750/1/70en_HK
dc.identifier.scopuseid_2-s2.0-84859902542en_HK
dc.identifier.hkuros199808en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-84859902542&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume750en_HK
dc.identifier.issue1en_HK
dc.identifier.eissn1538-4357-
dc.identifier.isiWOS:000303063500070-
dc.publisher.placeUnited Statesen_HK
dc.identifier.scopusauthoridTakata, J=22735157300en_HK
dc.identifier.scopusauthoridOkazaki, AT=7102544677en_HK
dc.identifier.scopusauthoridNagataki, S=55190607300en_HK
dc.identifier.scopusauthoridNaito, T=26024912200en_HK
dc.identifier.scopusauthoridKawachi, A=7004355934en_HK
dc.identifier.scopusauthoridLee, SH=54923631900en_HK
dc.identifier.scopusauthoridMori, M=36123616300en_HK
dc.identifier.scopusauthoridHayasaki, K=25225640600en_HK
dc.identifier.scopusauthoridYamaguchi, MS=7404824802en_HK
dc.identifier.scopusauthoridOwocki, SP=7003906613en_HK

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