Tidally Induced Outbursts in Oj 287 During 2005-2008

Valtonen, M. J.; Nilsson, K.; Villforth, C.; Lehto, H. J.; Takalo, L. O.; Lindfors, E.; Sillanpää, A.; Hentunen, V. P.; Mikkola, Seppo; Zoła, S.; Dróżdż, M.; Kozieł, D.; Ogłoza, W.; Kurpińska-Winiarska, M.; Siwak, M.; Winiarski, M.; Heidt, J.; Kidger, M.; Pursimo, T.; Wu, Ji; Zhou, Xu; Sadakane, Kozo; Marchev, D.; Nissinen, M.; Niarchos, P. G.; Liakos, A.; Gazeas, K.; Doğru, S.; Poyner, G.; Dietrich, M.; Assef, Roberto J.; Atlee, D. W.; Bird, Jonathan C.; DePoy, D. L.; Eastman, Jason D.; Peeples, Molly S.; Prieto, J. L.; Watson, Linda C.; Yee, Jennifer C.; Mattingly, A.; Ohlert, J.

doi:10.1088/0004-637x/698/1/781

Cited by 56 publications

(60 citation statements)

References 16 publications

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“…Perturbations in the AGN accretion disk can be used to explain continuum flux changes and subsequent spectral changes (i.e. Stalevski, Jovanovic, & Popovic 2008;Valtonen et al 2009;Popović et al 2014). The perturbation of the accretion disk induces disk instability, and amongst several mechanisms, thermal instability is commonly invoked to explain AGN luminosity variations.…”

Section: Perturbation Of Accretion Diskmentioning

confidence: 99%

Recoiling Supermassive Black Hole in Changing-look AGN Mrk 1018

Kim

Yoon

Evans

2018

ApJ

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The spectral type of Mrk 1018 changed from Type 1.9 to 1 and returned back to 1.9 over a period of 40 years. We have investigated physical mechanisms responsible for the spectral change in Mrk 1018 by analyzing archival spectral and imaging data. Two kinematically distinct broad-line components, blueshifted and redshifted components, are found from spectral decomposition. The velocity offset curve of the broad-line as a function of time shows a characteristic pattern. An oscillating recoiled supermassive black hole (rSMBH) scenario is proposed to explain the observed velocity offset in broad emission lines. A Bayesian Markov-Chain Monte Carlo simulation is performed to derive the best fit orbital parameters; we find that the rSMBH has a highly eccentric orbit with a period of ∼29 years. The AGN activity traced by variation of broad Hβ emission line is found to increase and decrease rapidly at the start and end of the cycle, and peaked twice at the start and near the end of the cycle. Extinction at the start and end of the cycle (when its spectral type is Type 1.9) is found to increase due to increased covering factor. Perturbations of the accretion disk caused by pericentric passage can reasonably explain the AGN activity and spectral change in Mrk 1018. Currently, the spectral type of Mrk 1018 is Type 1.9, and we do not know if it will repeat a similar pattern of spectral change in the future, but if it does, then spectral type will turn to Type 1 around mid 2020's.

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Section: Perturbation Of Accretion Diskmentioning

confidence: 99%

Recoiling Supermassive Black Hole in Changing-look AGN Mrk 1018

Kim

Yoon

Evans

2018

ApJ

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“…As the short time delay between the accretion disc piercing and the jet response is so fundamentally important for this model, we will discuss this point in greater detail. It is unclear why Valtonen et al (2009) chose this particular radius. For comparison, the radius at which the accreting material plunges into the black hole, the innermost stable circular orbit (ISCO) is R ISCO = 3 × R Schwarzschild for a non-rotating black hole.…”

Section: Lehto and Valtonen: A Binary Black Hole Two Disc Piercingsmentioning

confidence: 99%

“…The ISCO is the smallest radius at which the accreting material could enter the jet. Additionally, Valtonen et al (2009) did not take viscosity and MHD effects into account. Viscosity and turbulence play a major role in accretion processes (Balbus & Hawley 1998), and thus estimations neglecting these effects might yield wrong results.…”

Section: Lehto and Valtonen: A Binary Black Hole Two Disc Piercingsmentioning

confidence: 99%

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

Villforth

Nilsson

Heidt³

et al. 2010

Monthly Notices of the Royal Astronomical Society

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OJ 287 is a BL Lac object at redshift z= 0.306 that has shown double‐peaked bursts at regular intervals of ∼12 yr during the last ∼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.

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“…Sillanpää et al [13] (1996a [13], 1996b [14]) reported the next double-peak outburst occurrence in 1994-1995, which occurred almost exactly at the predicted times. Then a double-peaked outburst was also seen during the next recurrence in [2005][2006][2007][2008] [15]. These predicted recurrences are usually interpreted as OJ 287 housing a binary pair of black holes system with a period of ∼12 years.…”

Section: Introductionmentioning

confidence: 99%

Intra-Night Variability of OJ 287 with Long-Term Multiband Optical Monitoring

Zeng

Zhao²,

Jiang

et al. 2017

Galaxies

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Abstract:We present long-term optical multi-band photometric monitoring of the blazar OJ 287 from 6 March 2010 to 3 April 2016, with high temporal resolution in the VRI-bands. The flux variations and colour-magnitude variations on long and short timescales were investigated to understand the emission mechanisms. In our observation, the major outbursts occurred in January 2016, as predicted by the binary pair of black holes model for OJ 287, with F var of 1.3∼2.1%, and variability amplitude (Amp) of 5.8∼9.0%. The intra-night variability (IDV) durations were from 18.5 to 51.3 min, and the minimal variability timescale was about 4.7 min. The colour-magnitude variation showed a weak positive correlation on the long timescale with Pearson's r = 0.450, while a negative correlation was found on intra-night timescales. We briefly discuss the possible physical mechanisms that are most likely to be responsible for the observed flux and colour-magnitude correlation variability.

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Tidally Induced Outbursts in Oj 287 During 2005-2008

Cited by 56 publications

References 16 publications

Recoiling Supermassive Black Hole in Changing-look AGN Mrk 1018

Recoiling Supermassive Black Hole in Changing-look AGN Mrk 1018

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

Intra-Night Variability of OJ 287 with Long-Term Multiband Optical Monitoring

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