Probing Jet Launching in Neutron Star X-Ray Binaries: The Variable and Polarized Jet of SAX J1808.4-3658

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dc.contributor.authorBaglio M.C.
dc.contributor.authorRussell D.M.
dc.contributor.authorCrespi S.
dc.contributor.authorCovino S.
dc.contributor.authorJohar A.
dc.contributor.authorHoman J.
dc.contributor.authorBramich D.M.
dc.contributor.authorSaikia P.
dc.contributor.authorCampana S.
dc.contributor.authorD'Avanzo P.
dc.contributor.authorFender R.P.
dc.contributor.authorGoldoni P.
dc.contributor.authorGoodwin A.J.
dc.contributor.authorLewis F.
dc.contributor.authorMasetti N.
dc.contributor.authorZanon A.M.
dc.contributor.authorMotta S.E.
dc.contributor.authorMunoz-Darias T.
dc.contributor.authorShahbaz T.
dc.date.accessioned2021-08-03T22:22:03Z
dc.date.available2021-08-03T22:22:03Z
dc.date.issued2020-12
dc.descriptionIndexación Scopuses
dc.description.abstractWe report on an optical photometric and polarimetric campaign on the accreting millisecond X-ray pulsar (AMXP) x display--inline-block" style="background: var(--highlight-yellow); color: inherit;">SAX x display--inline-block" style="background: var(--highlight-yellow); color: inherit;">4-x display--inline-block" style="background: var(--highlight-yellow); color: inherit;">J1808.x display--inline-block" style="background: var(--highlight-yellow); color: inherit;">4-x display--inline-block" style="background: var(--highlight-yellow); color: inherit;">3658 during its 2019 outburst. The emergence of a low-frequency excess x display--inline-block" style="background: var(--highlight-yellow); color: inherit;">in the spectral energy distribution x display--inline-block" style="background: var(--highlight-yellow); color: inherit;">in the form of a red excess above the disk spectrum (seen most prominently x display--inline-block" style="background: var(--highlight-yellow); color: inherit;">in the z, i, and R bands) is observed as the outburst evolves. This is indicative of optically thin synchrotron emission due to a jet, as seen previously x display--inline-block" style="background: var(--highlight-yellow); color: inherit;">in this source and x display--inline-block" style="background: var(--highlight-yellow); color: inherit;">in other AMXPs during outburst. At the end of the outburst decay, the source enters a reflaring state. The low-frequency excess is still observed during the reflares. Our optical (BVRI) polarimetric campaign shows variable linear polarization (LP) throughout the outburst. We show that this is intrinsic to the source, with low-level but significant detections (0.2%-2%) x display--inline-block" style="background: var(--highlight-yellow); color: inherit;">in all bands. The LP spectrum is red during both the main outburst and the reflaring state, favoring a jet origin for this variable polarization over other interpretations, such as Thomson scattering with free electrons from the disk or the propelled matter. During the reflaring state, a few episodes with stronger LP levels (1%-2%) are observed. The low-level, variable LP is suggestive of strongly tangled magnetic fields near the base of the jet. These results clearly demonstrate how polarimetry is a powerful tool for x display--inline-block" style="background: var(--highlight-yellow); color: inherit;">probing the magnetic field structure x display--inline-block" style="background: var(--highlight-yellow); color: inherit;">in X-ray binary jets, as for active galactic nuclei jets. © 2020. The American Astronomical Society. All rights reserved..es
dc.description.urihttps://iopscience-iop-org.recursosbiblioteca.unab.cl/article/10.3847/1538-4357/abc685
dc.identifier.citationAstrophysical Journal, Volume 905, Issue 216 December 2020 Article number 87es
dc.identifier.doi10.3847/1538-4357/abc685
dc.identifier.issn0004637X
dc.identifier.urihttp://repositorio.unab.cl/xmlui/handle/ria/19641
dc.language.isoeses
dc.publisherIOP Publishing Ltd.es
dc.subjectBlack Holeses
dc.subjectCygnuses
dc.subjectOutburstes
dc.titleProbing Jet Launching in Neutron Star X-Ray Binaries: The Variable and Polarized Jet of SAX J1808.4-3658es
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