Optical polarization angle and VLBI jet direction in the binary black hole model of OJ287

Valtonen, M. J.; Wiik, K.

doi:10.1111/j.1365-2966.2011.20009.x

Cited by 44 publications

(62 citation statements)

References 48 publications

(72 reference statements)

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“…(Valtonen & Wiik 2012 had interchanged i and Ω by mistake; this, however, had no consequences in that paper apart from wrong labels. Correcting this error, the results agree with the present work.)…”

Section: The Inner Diskmentioning

confidence: 99%

“…Moreover, the 12-year cycle is clearly modulated by a longer time scale variation (Valtonen & Wiik 2012) even though it is too soon to claim that the 60-year cycle has also been detected since the radio jet observations cover only about 30 years, in contrast to the 120-year optical light curve. A new twist in the story is the radio jet measurements at mm waves: they show variations of much larger amplitude (Agudo et al 2012b;Tateyama 2013).…”

Section: Introductionmentioning

confidence: 99%

“…Considering that the period rotation of the innermost disk is about 0.5 yr, and that the viscous time scale of the inner disk is about an order of magnitude greater than this, the appropriate averaging time scale is in the range of 5 to 10 years (Krolik et al 2005). We use ten-year averaging (as in Valtonen & Wiik 2012) that lowers the coefficient A 2 from 2.24 to 0.75. The values for t 1 = 1903.9 and t 2 = 1893.5 are insensitive to the inclination i 0 and to the averaging time scale, while the value of C = 3.13 is of no importance to what follows.…”

Section: The Inner Diskmentioning

confidence: 99%

“…We placed a ring of particles around the primary, and starting from year 1856, followed the evolution of each disk particle. The calculations were carried out as in Valtonen & Wiik (2012): in the present simulation the number of disc particles is 1500. They were placed in circular orbits between 1.7 and 14 Schwarzschild radii of the primary.…”

Section: The Inner Diskmentioning

confidence: 99%

“…However, a combination of optical variability data together with the jet variations at these two frequency ranges provides enough challenging data to attempt a model. Valtonen & Wiik (2012) looked at the variations of the rotation axis of the inner accretion disk in the well-defined binary model which gives a detailed account of the optical variations (Valtonen et al 2008). They found that the disk shows a wobble in the 12-year time scale that could be associated with the jet variations at cm wavelengths.…”

Section: Introductionmentioning

confidence: 99%

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A helical jet model for OJ287

Valtonen

Pihajoki

2013

A&A

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Context. The quasar OJ287 has been under observation for over 120 years. The quasi-periodic nature of its optical light curve has led to a binary black hole model as a common explanation of the quasar. The radio jet of OJ287 has been under investigation for a shorter time, about 30 years. It has a complicated structure that varies dramatically over a time scale of a few years. Aims. Here we propose that this structure arises from a helical jet being observed from a small and varying viewing angle. The viewing angle variation is taken to be in tune with the binary orbital motion. Methods. We calculated the effect of the secondary black hole on the inner edge of the accretion disk of the primary using particle simulations. We presumed that the axis of the helix is perpendicular to the disk. We then followed the jet motion on its helical path and projected the jet to the sky plane. This projection was compared with observations both at mm waves and cm waves. Results. We find that this model reproduces the observations well if the changes in the axis of the conical helix propagate outwards with a relativistic speed of about 0.85c. In particular, this model explains at the same time the long-term optical brightness variations as varying Doppler beaming in a component close to the core, i.e., at parsec scale in real linear distance, while the mm and cm radio jet observations are explained as being due to jet wobble at much larger (100 parsec scale) distances from the core.

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Section: The Inner Diskmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: The Inner Diskmentioning

confidence: 99%

Section: The Inner Diskmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A helical jet model for OJ287

Valtonen

Pihajoki

2013

A&A

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A precessing and nutating jet in OJ287

Britzen

Fendt²,

Witzel³

et al. 2018

Proc. IAU

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We re-analyzed OJ287 in 120 Very Long Baseline Array (VLBA, MOJAVE) observations (at 15 GHz) covering the time span between Apr. 1995 and Apr. 2017. We find that the radio jet motion over the sky is consistent with a precessing and nutating jet source. The variability of the radio flux-density can be explained by Doppler beaming due to a change in the viewing angle. We suggest that part of the optical emission is due to synchrotron emission related to the jet radiation. We find a strikingly similar scaling for the timescales for precession and nutation as indicated for SS433 with a factor of roughly 50 times longer in OJ287.

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Possible quasi-periodic ejections in quasar B1308+326

Qian

Britzen

Witzel

et al. 2017

A&A

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Context. The search for periodic features in flux variability and kinematics of superluminal components in blazars is capable of providing significant clues for the understanding of the physical processes in their central engines (black-hole/accretion-disk systems), especially concerning the formation and structure of their relativistic jets and radiation mechanisms. Aims. The jet swing on parsec-scales and the change of the ejection position angle of the superluminal components with time in the quasar B1308+326 (z = 0.997) are investigated as quasi-periodic behaviors. Methods. A previously published precessing jet nozzle model is applied to model the source kinematics and a possible jet precession period is found. Results. Based on the model fitting of the kinematics for a subset of components, it is shown that their kinematics, including the shape of the inner trajectories and the motion of the components, could be well fitted in terms of the precessing jet nozzle model and a precession period of ∼16.9 ± 0.3 yr is derived. Different precession mechanisms are discussed and compared. Conclusions. It is shown that the swing of the ejection position angle of the superluminal knots observed in B1308+326 may be due to the orbital motion of a putative supermassive black hole binary in its nucleus. Some relevant parameters of the binary model are estimated. We also discuss the spin-induced precession mechanism in the single black hole scenario and an estimate for the spin of the Kerr black hole is obtained.

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Optical polarization angle and VLBI jet direction in the binary black hole model of OJ287

Cited by 44 publications

References 48 publications

A helical jet model for OJ287

A helical jet model for OJ287

A precessing and nutating jet in OJ287

Possible quasi-periodic ejections in quasar B1308+326

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