On the masses of OJ287 black holes

Valtonen, M. J.; Ciprini, S.; Lehto, H. J.

doi:10.1111/j.1365-2966.2012.21861.x

Cited by 85 publications

(88 citation statements)

References 73 publications

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“…If we do assume an angle offset of about 15 degrees, the calculated values match the observations. In this model the magnetic field of the optical emission region lies more or less parallel to the jet, as was also concluded in a previous work (Valtonen & Wiik 2012) internal extinction in the OJ287 host galaxy (Valtonen et al 2012a). Since the properties of the helix cone are now fully determined by the optical data, we may apply the model to radio data.…”

Section: The Helix Modelmentioning

confidence: 56%

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 Helix Modelmentioning

confidence: 56%

A helical jet model for OJ287

Valtonen

Pihajoki

2013

A&A

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“…The rotation about the common center and the piercing of the primary black hole accretion disk by the secondary black hole results in twin outbursts in the light-curve with a (quasi-) periodicity of about 12 yr (Valtonen et al 2012;Pihajoki 2014). The last outburst happened during the period of 2005-07, and was nicely traced.…”

Section: Oj287mentioning

confidence: 99%

Multi-wavelength Study of Blazars Using Variability as a Tool

Baliyan¹,

Kaur²,

Chandra³

et al. 2016

Journal of Astronomy and Space Sciences

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“…Based on the radio core size and the time delay between the radio band and γ-ray band, Karamanavis (2017) found that the γ-ray active region is located at 1.9±1.1 pc away from the jet base for PKS 1502+106, which is quite consistent with our estimates of ∼2 pc in this work. The correlation between the millimeter and the γ-ray light curves also indicates that the γ-ray emitting region should be located at >14 pc (Agudo et al 2011a) for OJ 287, which roughly corresponds to~R 10 4 S for the BH mass of ☉ M 10 10 (e.g., Valtonen et al 2012). …”

Section: Conclusion and Discussionmentioning

confidence: 99%

Constraints on the Location of γ-Ray Sample of Blazars with Radio Core-shift Measurements

Yan

et al. 2018

ApJ

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We model simultaneous or quasi-simultaneous multi-band spectral energy distributions (SEDs) for a sample of 25 blazars that have radio core-shift measurements, where a one-zone leptonic model and Markov chain Monte Carlo technique are adopted. In the SED fitting for 23 low-synchrotron-peaked (LSP) blazars, the seed photons from the broad-line (BLR) and molecular torus are considered respectively in the external Compton process. We find that the SED fitting with the seed photons from the torus are better than those utilizing BLR photons, which suggest that the γ-ray emitting region may be located outside the BLR. Assuming the magnetic field strength in the γ-ray emitting region as constrained from the SED fitting follows the magnetic field distribution as derived from the radio core-shift measurements (i.e.,1 , where R is the distance from the central engine and B 1 pc is the magnetic field strength at 1 pc), we further calculate the location of the γ-ray emitting region, g R , for these blazars. We find that~ǵ  R R R 2 10 10 4 S B L R (R S is the Schwarzschild radius and R BLR is the BLR size), where R BLR is estimated from the broad-line luminosities using the empirical correlations obtained using the reverberation mapping methods.

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On the masses of OJ287 black holes

Cited by 85 publications

References 73 publications

A helical jet model for OJ287

A helical jet model for OJ287

Multi-wavelength Study of Blazars Using Variability as a Tool

Constraints on the Location of γ-Ray Sample of Blazars with Radio Core-shift Measurements

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