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dc.contributor.authorMacDonald, Nicholas Royen_US
dc.contributor.authorJorstad, Svetlana G.en_US
dc.contributor.authorMarscher, Alan P.en_US
dc.date.accessioned2019-02-19T14:57:19Z
dc.date.available2019-02-19T14:57:19Z
dc.date.issued2017-11-20
dc.identifier.citationNR MacDonald, SG Jorstad, AP Marscher. 2017. "" Orphan" γ-ray Flares and Stationary Sheaths of Blazar Jets." The Astrophysical Journal, Volume 850, Issue 1, https://doi.org/10.3847/1538-4357/aa92c8
dc.identifier.issn0004-637X
dc.identifier.urihttps://hdl.handle.net/2144/33335
dc.description.abstractBlazars exhibit flares across the entire electromagnetic spectrum. Many γ-ray flares are highly correlated with flares detected at longer wavelengths; however, a small subset appears to occur in isolation, with little or no correlated variability at longer wavelengths. These "orphan" γ-ray flares challenge current models of blazar variability, most of which are unable to reproduce this type of behavior. MacDonald et al. have developed the Ring of Fire model to explain the origin of orphan γ-ray flares from within blazar jets. In this model, electrons contained within a blob of plasma moving relativistically along the spine of the jet inverse-Compton scatter synchrotron photons emanating off of a ring of shocked sheath plasma that enshrouds the jet spine. As the blob propagates through the ring, the scattering of the ring photons by the blob electrons creates an orphan γ-ray flare. This model was successfully applied to modeling a prominent orphan γ-ray flare observed in the blazar PKS 1510−089. To further support the plausibility of this model, MacDonald et al. presented a stacked radio map of PKS 1510−089 containing the polarimetric signature of a sheath of plasma surrounding the spine of the jet. In this paper, we extend our modeling and stacking techniques to a larger sample of blazars: 3C 273, 4C 71.01, 3C 279, 1055+018, CTA 102, and 3C 345, the majority of which have exhibited orphan γ-ray flares. We find that the model can successfully reproduce these flares, while our stacked maps reveal the existence of jet sheaths within these blazars.en_US
dc.language.isoen_US
dc.publisherAmerican Astronomical Societyen_US
dc.relation.ispartofThe Astrophysical Journal
dc.rights© 2017. The American Astronomical Society. All rights reserved.en_US
dc.subjectScience & technologyen_US
dc.subjectPhysical sciencesen_US
dc.subjectAstronomy & astrophysicsen_US
dc.subjectGalaxies: activeen_US
dc.subjectGalaxies: jetsen_US
dc.subjectPolarizationen_US
dc.subjectRadiation mechanisms: non-thermalen_US
dc.subjectRelativistic processesen_US
dc.subjectTechniques: interferometricen_US
dc.subjectHelical magnetic-fielden_US
dc.subjectInner jeten_US
dc.subjectPolarizationen_US
dc.subject3C-273en_US
dc.subjectAstronomical and space sciencesen_US
dc.subjectOrganic chemistryen_US
dc.subjectPhysical chemistry (incl. structural)en_US
dc.title" Orphan" γ-ray flares and stationary sheaths of blazar jetsen_US
dc.typeArticleen_US
dc.description.versionAccepted manuscripten_US
dc.identifier.doi10.3847/1538-4357/aa92c8
pubs.elements-sourcemanual-entryen_US
pubs.notesEmbargo: No embargoen_US
pubs.organisational-groupBoston Universityen_US
pubs.organisational-groupBoston University, College of Arts & Sciencesen_US
pubs.organisational-groupBoston University, College of Arts & Sciences, Department of Astronomyen_US
pubs.publication-statusPublisheden_US
dc.identifier.orcid0000-0001-7396-3332 (Marscher, AP)


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