Property Study of Oj 287 and Bl Lac Variability in Opticaland Radio Ranges

Sukharev, A. L.; Ryabov, M. I.; Bezrukovs, Vladislavs

doi:10.15407/rpra24.04.254

Cited by 5 publications

(7 citation statements)

References 26 publications

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“…This period washed out the period of about 6 years, obtained previously using shorter data set [23]. We also note that the periods obtained from the total radio flux density (≈25 years [21,22]) and from the motion of the jet ridgeline (≈22 years [15]) are consistent. The periodicity of ≈1 year is found in both optical and radio domains [15,22].…”

Section: Introductionsupporting

confidence: 85%

“…None of the above models can consistently explain the main observable facts: (i) the sudden change in PA in which was first detected at 43 GHz in 2004 [28,36] and about six years later at 15 GHz; (ii) the difference of the long-term variability period in optical (≈12 yr [1]) and radio (≈25 yr [21][22][23]) flux densities.…”

Section: Discussionmentioning

confidence: 92%

“…Hence, in measurements of the total radio flux density from the entire source, the periodicity cannot be strongly obscured by radiation from the optically thin part of the jet. Statistical analysis performed in [21,22] based on data from the Owens Valley Radio Observatory (OVRO, 2008(OVRO, −2018 and Radio Astronomy Observatory of Michigan University (UMRAO, 1974(UMRAO, −2011 shows that the period of long-term radio variability is about 25 years. This period washed out the period of about 6 years, obtained previously using shorter data set [23].…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Is OJ 287 a Single Supermassive Black Hole?

Butuzova

Pushkarev

2020

Universe

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Light curves for more than century optical photometric observations of the blazar OJ 287 reveals strong flares with a quasi-period of about 12 years. For a long time, this period has been interpreted by processes in a binary black hole system. We propose an alternative explanation for this period, which is based on Doppler factor periodic variations of the emitting region caused by jet helicity. Using multi-epoch very large baseline interferometry (VLBI) observations carried out in a framework of the MOJAVE (Monitoring Of Jets in Active galactic nuclei with VLBA Experiments) program and other VLBA (Very Long Baseline Array) archival experiments at the observing frequency of 15 GHz, we derived geometrical parameters of the jet helix. To reach an agreement between the VLBI and photometric optical observation data, the jet component motion at a small angle to the radial direction is necessary. Such non-radial motion is observed and, together with the jet helical shape, can be naturally explained by the development of the Kelvin–Helmholtz instability in the parsec-scale outflow. In this case, the true precession of the OJ 287 jet may manifest itself in differences between the peak flux values of the 12-year optical flares. A possibility to create this precession due to Lense–Thirring effect of a single supermassive black hole is also discussed.

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Section: Introductionsupporting

confidence: 85%

Section: Discussionmentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Is OJ 287 a Single Supermassive Black Hole?

Butuzova

Pushkarev

2020

Universe

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“…The precession period, determined by optical data of 12 years, does not appear in the light curves in the radio range. Moreover, the periods of the radio flux variability and change in the inner jet PA approximately correspond to both each other and ≈ 25 − 30 years (Britzen et al 2018;Ryabov et al 2016;Sukharev et al 2019), and allow us to correlate their formation with the jet helical shape due to precession. These periods are significantly smaller than the periods found here.…”

Section: Precession Of the Kpc-scale Jetmentioning

confidence: 69%

The blazar OJ 287 jet from parsec- to kiloparsec-scales

Butuzova

2021

Preprint

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The curved shape of the kiloparsec-scale jet of the blazar OJ 287 is analyzed in the framework of the precession of the central engine, on the existence on which a large number of studies over the past decades are based. The data necessary for the analysis on the kiloparsec-scale jet velocity and angle with the line of sight are obtained based on two competing assumptions about the X-ray emission mechanism of the OJ 287 jet. Namely, there were both the inverse Compton scattering of the microwave background under the assumption of relativistic kiloparsec-scale jet and the inverse Compton scattering of the central source radiation. For the latter one, we showed that the expected flux from the kiloparsec-scale jet in the gamma range does not exceed the limit set for it according to Fermi -LAT data. We found that only the period of the kiloparsec-scale jet helix, estimated in the framework of the inverse Compton scattering of the central source radiation, agrees with the precession period of the central engine, determined from the modulation of the peak values of 12-year optical flares.

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“…The precession period, determined by optical data of 12 years, does not appear in the light curves in the radio range. Moreover, the periods of the radio flux variability and change in the inner jet PA approximately correspond to both each other and ≈25-kpc IC CMB kpc 8 1 T 30 years [14,40,41], and allow us to correlate their formation with the jet helical shape due to precession. These periods are significantly smaller than the periods found here.…”

Section: F(ω)mentioning

confidence: 90%

The Blazar OJ 287 Jet from Parsec to Kiloparsec Scales

Butuzova

2021

Astron. Rep.

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The curved shape of the kiloparsec-scale jet of the blazar OJ 287 is analyzed in the framework of the precession of the central engine, on the existence on which a large number of studies over the past decades are based. The data necessary for the analysis on the kiloparsec-scale jet velocity and angle with the line of sight are obtained based on two competing assumptions about the X-ray emission mechanism of the OJ 287 jet. Namely, there were both the inverse Compton scattering of the cosmic microwave background under the assumption of relativistic kiloparsec-scale jet and the inverse Compton scattering of the central source radiation. For the latter one, we showed that the expected flux from the kiloparsec-scale jet in the gamma range does not exceed the limit set for it according to Fermi-LAT data. We found that only the period of the kiloparsec-scale jet helix, estimated in the framework of the inverse Compton scattering of the central source radiation, agrees with the precession period of the central engine, determined from the modulation of the peak values of 12‑year optical flares.

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Property Study of Oj 287 and Bl Lac Variability in Opticaland Radio Ranges

Cited by 5 publications

References 26 publications

Is OJ 287 a Single Supermassive Black Hole?

Is OJ 287 a Single Supermassive Black Hole?

The blazar OJ 287 jet from parsec- to kiloparsec-scales

The Blazar OJ 287 Jet from Parsec to Kiloparsec Scales

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