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Article: Stationary accelerators around Keplerian disks of aligned magnetized collapsed objects: Pair production and gamma-ray emission

TitleStationary accelerators around Keplerian disks of aligned magnetized collapsed objects: Pair production and gamma-ray emission
Authors
KeywordsGamma Rays: General
Hydromagnetics
Pulsars
Stars: Accretion
Stars: Collapsed
Stars: Rotation
X-Rays: Binaries
Issue Date1991
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 1991, v. 373 n. 1, p. 187-197 How to Cite?
AbstractThe magnetosphere is described for a system consisting of a spinning collapsed star connected by an aligned magnetic dipole field (B) to a surrounding idealized coaxial, nonviscous cool Keplerian disk. When the inner part of the conducting disk rotates more rapidly than the star, the magnetosphere is charge-separated. A part of the magnetosphere will corotate either with the star or with that part of the disk to which it is linked by the magnetic field. Separating such differently rotating regions are "gaps" empty of plasma. The magnetic field, including that part which penetrates through the disk, remains everywhere time-independent. Except in the gap and in the disk, the electric field component is E·B ≅ 0. The dynamo electromotive force from the (differently) rotating star and disk connected by B is balanced by the potential drop along B in the gap. The model gap potential drop is about 10 16 V for disk and star parameters of a low-mass X-ray binary (LMXB) and about 10 15 V for those of typical X-ray pulsar binaries. If very hot plasma from the star or the disk does not quench the accelerator, accretion-powered X-rays which traverse the gap limit its accelerating electric field by the e ± pair-production processes which they support. In the resulting steady state a constant current flows through the accelerator which gives a twist to, but does not continually stretch, the magnetic field through the disk. The steady state gap potential drop can accelerate proton (ions) toward the disk with enough energy so that interactions in the disk can give TeV y-rays. For LMXB parameters the model gives strong e ± production and hard X-ray and MeV γ-ray emission with total power near that of accretion-powered X-rays. With X-ray pulsar binary parameters the model total γ-ray power is typically about 10 -2 times the full accretion X-ray power. Possible application to disks around magnetic white dwarfs is considered.
Persistent Identifierhttp://hdl.handle.net/10722/175123
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_US
dc.contributor.authorRuderman, Men_US
dc.date.accessioned2012-11-26T08:49:20Z-
dc.date.available2012-11-26T08:49:20Z-
dc.date.issued1991en_US
dc.identifier.citationAstrophysical Journal Letters, 1991, v. 373 n. 1, p. 187-197en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/175123-
dc.description.abstractThe magnetosphere is described for a system consisting of a spinning collapsed star connected by an aligned magnetic dipole field (B) to a surrounding idealized coaxial, nonviscous cool Keplerian disk. When the inner part of the conducting disk rotates more rapidly than the star, the magnetosphere is charge-separated. A part of the magnetosphere will corotate either with the star or with that part of the disk to which it is linked by the magnetic field. Separating such differently rotating regions are "gaps" empty of plasma. The magnetic field, including that part which penetrates through the disk, remains everywhere time-independent. Except in the gap and in the disk, the electric field component is E·B ≅ 0. The dynamo electromotive force from the (differently) rotating star and disk connected by B is balanced by the potential drop along B in the gap. The model gap potential drop is about 10 16 V for disk and star parameters of a low-mass X-ray binary (LMXB) and about 10 15 V for those of typical X-ray pulsar binaries. If very hot plasma from the star or the disk does not quench the accelerator, accretion-powered X-rays which traverse the gap limit its accelerating electric field by the e ± pair-production processes which they support. In the resulting steady state a constant current flows through the accelerator which gives a twist to, but does not continually stretch, the magnetic field through the disk. The steady state gap potential drop can accelerate proton (ions) toward the disk with enough energy so that interactions in the disk can give TeV y-rays. For LMXB parameters the model gives strong e ± production and hard X-ray and MeV γ-ray emission with total power near that of accretion-powered X-rays. With X-ray pulsar binary parameters the model total γ-ray power is typically about 10 -2 times the full accretion X-ray power. Possible application to disks around magnetic white dwarfs is considered.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.subjectGamma Rays: Generalen_US
dc.subjectHydromagneticsen_US
dc.subjectPulsarsen_US
dc.subjectStars: Accretionen_US
dc.subjectStars: Collapseden_US
dc.subjectStars: Rotationen_US
dc.subjectX-Rays: Binariesen_US
dc.titleStationary accelerators around Keplerian disks of aligned magnetized collapsed objects: Pair production and gamma-ray emissionen_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-s2.0-4243683307en_US
dc.identifier.volume373en_US
dc.identifier.issue1en_US
dc.identifier.spage187en_US
dc.identifier.epage197en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US
dc.identifier.scopusauthoridRuderman, M=7006487382en_US

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