Accretion Disk Parameters Determined from the Great 2015 Flare of OJ 287

Valtonen, M. J.; Zoła, S.; Pihajoki, Pauli; Enestam, S.; Lehto, H. J.; Dey, Lankeswar; Gopakumar, A.; Dróżdż, M.; Ogłoza, W.; Żejmo, M.; Gupta, Alok C.; Pursimo, T.; Ciprini, S.; Kidger, M.; Nilsson, K.; Berdyugin, A.; Piirola, V.; Jermak, Helen; Hudec, R.; Laine, Seppo

doi:10.3847/1538-4357/ab3573

Cited by 42 publications

(62 citation statements)

References 44 publications

(96 reference statements)

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“…This model requires further verification by magnetohydrodynamic simulations. The maximum flux density of the last 12-year flare occurred in 2016 was 17 mJy in B band [42]. It is slightly higher than the ones for two previous flares ( Table 3).…”

Section: Discussionmentioning

confidence: 61%

“…Table 3. Used observational data [14,42] and obtained values of the angle between the cone axis and the line of sight θ 0 : the columns contain 1 Year F max , mJy F min , mJy θ 0 , deg Epoch (yr) ( deg ) Figure 9. Changes of the angle between the jet helix axis with the line of sight θ 0 due to the precession of the OJ 287 jet.…”

Section: Helical Jet Precessionmentioning

confidence: 99%

“…According to the broad-band observations, black hole masses for BL Lacertae objects were estimated as ∼(10 8 -10 9 ) M ( [44,45], and references therein). Valtonen et al [42] derived the primary black hole mass of ∼ 10 10 M under the assumption of the binary black hole system in the OJ 287 centre. This mass estimation is model-dependent, but we took it as an upper limit.…”

Section: Helical Jet Precessionmentioning

confidence: 99%

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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: Discussionmentioning

confidence: 61%

Section: Helical Jet Precessionmentioning

confidence: 99%

Section: Helical Jet Precessionmentioning

confidence: 99%

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Is OJ 287 a Single Supermassive Black Hole?

Butuzova

Pushkarev

2020

Universe

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“…The hadronic model, on the other hand, mainly focuses on the interpretation of the MeV-GeV emission and the NIR-optical break remains unexplained. Neither the optically thin bremsstrahlung emission from a 25eV thermal plasma responsible for QPOOs, as argued in Valtonen et al [101] is consistent with the NIR-optical break though it may have a sub-dominant contribution. Optically thin bremsstrahlung emissivity has a spectral index of ∼ 0 (F ν ∼ ν −a ).…”

Section: Discussionmentioning

confidence: 74%

A Multi-Wavelength View of OJ 287 Activity in 2015–2017: Implications of Spectral Changes on Central-Engine Models and MeV-GeV Emission Mechanism

Kushwaha

2020

Galaxies

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A diverse range of observational results and peculiar properties across the domains of observation have made OJ 287 one of the best-explored BL Lac objects on the issues of relativistic jets and accretion physics as well as the strong theory of gravity. We here present a brief compilation of observational results from the literature and inferences/insights from the extensive studies but focus on the interpretation of its ∼ 12-yr quasi-periodic optical outbursts (QPOOs) and high energy emission mechanisms. The QPOOs in one model are attributed to the disk-impact related to dynamics of the binary SMBHs while alternative models attribute it to the geometrical effect related to the precession of a single jet or double jets. We discuss implications of the new spectral features reported during the 2015-2017 multi-wavelength high activity of the source -a break in the NIR-optical spectrum and hardening of the MeV-GeV emission accompanied by a shift in the location of its peak, in the context of the two. The reported NIR-optical break nicely fits the description of a standard accretion disk emission from an SMBH of mass ∼ 10 10 M while the time of its first appearance in end-May 2013 (MJD 56439) is in close coincidence with the time of impact predicted by the disk-impact binary SMBH model. This spectral and temporal coincidence with the model parameters of the disk-impact binary SMBH model provides independent evidence in favor of the model over the geometrical models which argue a total central-engine mass in the range of 10 7−9 M . On the other hand, the MeV-GeV spectral change is naturally reproduced by the inverse Compton scattering of photons from the broad-line region and is consistent with the detection of broad emission lines during the previous cycles of quasi-periodic outbursts. Combining this with previous SED studies suggests that in OJ 287, MeV-GeV emission results from external Comptonization. 2 of 21 minutes and even less to decades 1 [∼ 6-7 orders of magnitude; e.g. 2]. Their radio and optical emission is highly polarized and have been observed to vary often with the source flux, all the way from 0 to > 50%. Imaging in radio, infra-red (IR), optical, and X-ray, on the other hand, show an extremely well collimated jet extending up to Mpc scales [∼ 9-13 orders of magnitude; e.g. 3,4] with frequent sighting of superluminal features in high-resolution imaging of the core. Taken together with the observational and theoretical understanding of other astrophysical objects combined with their high and rarely repeating observational behavior indicates that they are the site of complex, multi-level, multi-scale physics and thus, are normally called extreme sources among non-catastrophic events.Though studies in different energy bands finally culminated into a unified scheme for radio-loud AGNs [5], it also revealed that AGNs need well-coordinated multi-wavelength (MW) observations to go beyond the limits associated with individual bands. The launch of the gamma-ray survey observatory Fermi-LAT (Large Area Telescope...

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“…These flares arise due to the impact of an orbiting secondary BH onto the accretion disk of the primary. In the resulting thermal flares, flux densities (hereafter "flux") in the UV-infrared wavelengths increase sharply within just a day or so and then fall off more slowly in the following days (Valtonen et al 2019). Accurate timing of these flares allows us to track the general relativistic trajectory of the secondary BH and to determine BBH central engine parameters (Dey et al 2018, hereafter D18).…”

Section: Introductionmentioning

confidence: 99%

Spitzer Observations of the Predicted Eddington Flare from Blazar OJ 287

Laine

Dey

Valtonen

et al. 2020

ApJL

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Binary black hole (BH) central engine description for the unique blazar OJ287 predicted that the next secondary BH impact-induced bremsstrahlung flare should peak on 2019 July 31. This prediction was based on detailed general relativistic modeling of the secondary BH trajectory around the primary BH and its accretion disk. The expected flare was termed the Eddington flare to commemorate the centennial celebrations of now-famous solar eclipse observations to test general relativity by Sir Arthur Eddington. We analyze the multi-epoch Spitzer observations of the expected flare between 2019 July 31 and 2019 September 6, as well as baseline observations during 2019 February-March. Observed Spitzer flux density variations during the predicted outburst time display a strong similarity with the observed optical pericenter flare from OJ287 during 2007 September. The predicted flare appears comparable to the 2007 flare after subtracting the expected higher base-level Spitzer flux densities at 3.55 and 4.49 μm compared to the optical R-band. Comparing the 2019 and 2007 outburst lightcurves and the previously calculated predictions, we find that the Eddington flare arrived within 4 hr of the predicted time. Our Spitzer observations are well consistent with the presence of a nano-Hertz gravitational-wave emitting spinning massive binary BH that inspirals along a general relativistic eccentric orbit in OJ287. These multi-epoch Spitzer observations provide a parametric constraint on the celebrated BH no-hair theorem. Unified Astronomy Thesaurus concepts: Gravitation (661); Black hole physics (159); BL Lacertae objects (158)

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Accretion Disk Parameters Determined from the Great 2015 Flare of OJ 287

Cited by 42 publications

References 44 publications

Is OJ 287 a Single Supermassive Black Hole?

Is OJ 287 a Single Supermassive Black Hole?

A Multi-Wavelength View of OJ 287 Activity in 2015–2017: Implications of Spectral Changes on Central-Engine Models and MeV-GeV Emission Mechanism

Spitzer Observations of the Predicted Eddington Flare from Blazar OJ 287

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