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Article: A Model for AR Scorpii: Emission from Relativistic Electrons Trapped by Closed Magnetic Field Lines of Magnetic White Dwarfs

TitleA Model for AR Scorpii: Emission from Relativistic Electrons Trapped by Closed Magnetic Field Lines of Magnetic White Dwarfs
Authors
Keywordsbinaries: close
magnetic reconnection
methods: numerical
radiation mechanisms: non-thermal
white dwarfs
Issue Date2017
PublisherAmerican Astronomical Society, co-published with Institute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/
Citation
The Astrophysical Journal, 2017, v. 851 n. 2, p. 143:1-13 How to Cite?
AbstractAR Scorpii is an intermediate polar binary system composed of a magnetic white dwarf (WD) and an M-type star and shows nonthermal, pulsed, and highly linearly polarized emission. The radio/optical emission modulates with the WD's spin and shows the double-peak structure in the light curves. In this paper, we discuss a possible scenario for the radiation mechanism of AR Scorpii. The magnetic interaction on the surface of the companion star produces an outflow from the companion star, the heating of the companion star surface, and the acceleration of electrons to a relativistic energy. The accelerated electrons, whose typical Lorentz factor is ∼50-100, from the companion star move along the magnetic field lines toward the WD surface. The electrons injected with the pitch angle of sin θp,0 > 0.05 are subject to the magnetic mirror effect and are trapped in the closed magnetic field line region. We find that the emission from the first magnetic mirror points mainly contributes to the observed pulsed emission and the formation of the double-peak structure in the light curve. For the inclined rotator, the pulse peak in the calculated light curve shifts the position in the spin phase, and a Fourier analysis exhibits a beat frequency feature, which are consistent with the optical/UV observations. The pulse profile also evolves with the orbital phase owing to the effect of the viewing geometry. The model also interprets the global features of the observed spectral energy distribution in radio to X-ray energy bands. We also discuss the curvature radiation and the inverse-Compton scattering process in the outer gap accelerator of the WD in AR Scorpii and the possibility of the detection by future high-energy missions.
Persistent Identifierhttp://hdl.handle.net/10722/250563
ISSN
2019 Impact Factor: 5.745
2015 SCImago Journal Rankings: 3.266
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorTakata, J-
dc.contributor.authorYang, H-
dc.contributor.authorCheng, KS-
dc.date.accessioned2018-01-18T04:29:02Z-
dc.date.available2018-01-18T04:29:02Z-
dc.date.issued2017-
dc.identifier.citationThe Astrophysical Journal, 2017, v. 851 n. 2, p. 143:1-13-
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10722/250563-
dc.description.abstractAR Scorpii is an intermediate polar binary system composed of a magnetic white dwarf (WD) and an M-type star and shows nonthermal, pulsed, and highly linearly polarized emission. The radio/optical emission modulates with the WD's spin and shows the double-peak structure in the light curves. In this paper, we discuss a possible scenario for the radiation mechanism of AR Scorpii. The magnetic interaction on the surface of the companion star produces an outflow from the companion star, the heating of the companion star surface, and the acceleration of electrons to a relativistic energy. The accelerated electrons, whose typical Lorentz factor is ∼50-100, from the companion star move along the magnetic field lines toward the WD surface. The electrons injected with the pitch angle of sin θp,0 > 0.05 are subject to the magnetic mirror effect and are trapped in the closed magnetic field line region. We find that the emission from the first magnetic mirror points mainly contributes to the observed pulsed emission and the formation of the double-peak structure in the light curve. For the inclined rotator, the pulse peak in the calculated light curve shifts the position in the spin phase, and a Fourier analysis exhibits a beat frequency feature, which are consistent with the optical/UV observations. The pulse profile also evolves with the orbital phase owing to the effect of the viewing geometry. The model also interprets the global features of the observed spectral energy distribution in radio to X-ray energy bands. We also discuss the curvature radiation and the inverse-Compton scattering process in the outer gap accelerator of the WD in AR Scorpii and the possibility of the detection by future high-energy missions.-
dc.languageeng-
dc.publisherAmerican Astronomical Society, co-published with Institute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/-
dc.relation.ispartofThe Astrophysical Journal-
dc.rightsThe Astrophysical Journal. Copyright © American Astronomical Society, co-published with Institute of Physics Publishing, Inc.-
dc.subjectbinaries: close-
dc.subjectmagnetic reconnection-
dc.subjectmethods: numerical-
dc.subjectradiation mechanisms: non-thermal-
dc.subjectwhite dwarfs-
dc.titleA Model for AR Scorpii: Emission from Relativistic Electrons Trapped by Closed Magnetic Field Lines of Magnetic White Dwarfs-
dc.typeArticle-
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hk-
dc.identifier.authorityCheng, KS=rp00675-
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.3847/1538-4357/aa9b33-
dc.identifier.scopuseid_2-s2.0-85039713671-
dc.identifier.hkuros284051-
dc.identifier.volume851-
dc.identifier.issue2-
dc.identifier.spage143:1-
dc.identifier.epage13-
dc.identifier.isiWOS:000418661900005-
dc.publisher.placeUnited States-
dc.identifier.issnl0004-637X-

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