Variability and stability in blazar jets on time-scales of years: optical polarization monitoring of OJ 287 in 2005-2009

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dc.authoridAtlee, David/0000-0002-7564-4121
dc.authoridDePoy, Darren/0000-0002-2581-9309
dc.authoridDrozdz, Marek/0000-0001-9587-1615
dc.authoridYee, Jennifer/0000-0001-9481-7123
dc.authoridPrieto, Jose/0000-0003-1072-2712
dc.authoridAssef, Roberto/0000-0002-9508-3667
dc.authoridGazeas, Kosmas/0000-0002-8855-3923
dc.contributor.authorVillforth, C.
dc.contributor.authorNilsson, K.
dc.contributor.authorHeidt, J.
dc.contributor.authorTakalo, L. O.
dc.contributor.authorPursimo, T.
dc.contributor.authorBerdyugin, A.
dc.contributor.authorLindfors, E.
dc.date.accessioned2025-01-27T20:58:00Z
dc.date.available2025-01-27T20:58:00Z
dc.date.issued2010
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractOJ 287 is a BL Lac object at redshift z = 0.306 that has shown double-peaked bursts at regular intervals of similar to 12 yr during the last similar to 40 yr. We analyse optical photopolarimetric monitoring data from 2005 to 2009, during which the latest double-peaked outburst occurred. The aim of this study is twofold: firstly, we aim to analyse variability patterns and statistical properties of the optical polarization light curve. We find a strong preferred position angle in optical polarization. The preferred position angle can be explained by separating the jet emission into two components: an optical polarization core and chaotic jet emission. The optical polarization core is stable on time-scales of years and can be explained as emission from an underlying quiescent jet component. The chaotic jet emission sometimes exhibits a circular movement in the Stokes plane. We find six such events, all on the time-scales of 10-20 d. We interpret these events as a shock front moving forwards and backwards in the jet, swiping through a helical magnetic field. Secondly, we use our data to assess different binary black hole models proposed to explain the regularly appearing double-peaked bursts in OJ 287. We compose a list of requirements a model has to fulfil to explain the mysterious behaviour observed in OJ 287. The list includes not only characteristics of the light curve but also other properties of OJ 287, such as the black hole mass and restrictions on accretion flow properties. We rate all existing models using this list and conclude that none of the models is able to explain all observations. We discuss possible new explanations and propose a new approach to understanding OJ 287. We suggest that both the double-peaked bursts and the evolution of the optical polarization position angle could be explained as a sign of resonant accretion of magnetic field lines, a 'magnetic breathing' of the disc.
dc.description.sponsorshipPolish MNiSW [381//H03/200/6]; Chinese National Natural Science Foundation [10603006, 10633020]; UK Science and Technology Facilities Council; STFC [ST/G009465/1] Funding Source: UKRI
dc.description.sponsorshipThe authors would like to thank the anonymous referee for his comments and suggestions. We would also like to thank Staszek Zola, Merja Tornikoski, Anne Lahteenmaki, the Metsahovi monitoring team, Esko Valtaoja and Vilppu Piirola. Part of the data presented here are based on observations made with the NOT, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrosica de Canarias. Part of the data presented here have been taken using ALFOSC, which is owned by the Instituto de Astrofisica de Andalucia (IAA) and operated at the NOT under agreement between IAA and the NBIfAFG of the Astronomical Observatory of Copenhagen. This paper is based on observations collected at the Centro Astronomico Hispano Aleman (CAHA) at CA, operated jointly by the Max-Planck Institut fur Astronomie and the Instituto de Astrofisica de Andalucia (CSIC). This work was partly supported by the Polish MNiSW grant No. 381//H03/200/6. Jianghua Wu and Xu Zhou are supported by the Chinese National Natural Science Foundation grants 10603006 and 10633020. Part of the data presented here have been taken using the Liverpool Telescope, operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council.
dc.identifier.doi10.1111/j.1365-2966.2009.16133.x
dc.identifier.endpage2111
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.issue3
dc.identifier.scopus2-s2.0-77949337273
dc.identifier.scopusqualityQ1
dc.identifier.startpage2087
dc.identifier.urihttps://doi.org/10.1111/j.1365-2966.2009.16133.x
dc.identifier.urihttps://hdl.handle.net/20.500.12428/26577
dc.identifier.volume402
dc.identifier.wosWOS:000274483500059
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherOxford Univ Press
dc.relation.ispartofMonthly Notices of The Royal Astronomical Society
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WoS_20250125
dc.subjectaccretion
dc.subjectaccretion discs
dc.subjectmagnetic fields
dc.subjectpolarization
dc.subjectshock waves
dc.subjectBL Lacertea objects: individual: OJ 287
dc.subjectgalaxies: jets
dc.titleVariability and stability in blazar jets on time-scales of years: optical polarization monitoring of OJ 287 in 2005-2009
dc.typeArticle

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