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OJ 287

Coordinates:Sky map08h54m48.9s,+20° 06′ 31″
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OJ 287
Comparisons of large and small black holes in galaxy OJ 287 to theSolar System
Observation data(EpochJ2000)
ConstellationCancer
Right ascension08h54m48.9s[1]
Declination+20° 06′ 31″[1]
Redshift0.306000[1]
Distance4Gly(1.226Gpc)
TypeBL Lac[1]
Apparent magnitude(V)15.43[2]
Other designations
EGO 0851+202,[1]3EG J0853+1941,[1]RGB J0854+201[1]
See also:Quasar,List of quasars

OJ 287is aBL Lac object4billionlight-yearsfrom Earth that has produced quasi-periodic optical outbursts going back approximately 120 years, as first apparent on photographic plates from 1891. Seen on photographic plates since at least 1887,[3]it was first detected at radio wavelengths during the course of theOhio Sky Survey.It is asupermassive black holebinary (SMBHB).[4]The intrinsic brightness of the flashes corresponds to over a trillion times the Sun's luminosity, greater than the entire Milky Way galaxy's light output.[5]

Characteristics[edit]

Given the variability in the SMBHB's bursts and properties, multiple models have been proposed to account for these flashes. The initial model estimates the mass of the primary black hole to be approximately 18.35 billionsolar massesand the secondary black hole around 150 million solar masses. More recent models estimate that the central supermassive black hole has a mass of 100 million solar masses,[6]much less than previous estimations. This would make itsSchwarzschild radiusabout 1.97 AU.

Black Hole Disk Flares In Galaxy OJ 287 (1:22; animation; 28 April 2020)
Interferometric observations of OJ287 by theVLBAresolved with theCHIRPalgorithm and another algorithm by a group from Boston university.[7]OJ287 is a target candidate of the Event Horizon Telescope,3C279wastargetedby it in 2017.

The optical light curve shows that OJ 287 has a periodic variation of 11–12 years with a narrow double peak at maximum brightness.[8]This kind of variation suggests that it is abinary supermassive black hole.[9]The double-burst variability is thought to result from the smallerblack holepunching through theaccretion discof the larger black hole twice in every 12 years.[5]

A secondary black hole orbits the larger one with an observed orbital period of approximately 12 years and a calculatedeccentricityof approximately 0.65.[4]The maximum brightness is obtained when the minor component moves through theaccretion diskof the supermassive component atperinigricon.The perinigricon and aponigricon of its orbit are about 3,250 and 17,500 AU. In recent models, the mass of the secondarysupermassive black holehas been estimated to be approximately 125 million solar masses, although this has been debated through multiple studies.

An international research group, led by Stefanie Komossa, calculated the mass of the primary black hole. "The results show that an exceptionally massive black hole exceeding 10 billion solar masses is no longer needed...the results favor models with a smaller mass of 100 million solar masses for the primary black hole".[6]

In order to reproduce all the known outbursts, the rotation of the primary black hole is calculated to be 38% of themaximum allowed rotationfor aKerr black hole.[10][4]

The companion's orbit is decaying via the emission ofgravitational radiationand it is expected to merge with the central black hole within approximately 10,000 years.[11][12][13]

References[edit]

  1. ^abcdefg"NED results for object OJ +287".NASA/IPAC Extragalactic Database.Retrieved2008-07-10.
  2. ^"QSO J0854+2006".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved15 March2018.
  3. ^Camille M. Carlisle (13 January 2015)."Black Hole Binary En Route to Merger?".Sky & Telescope.
  4. ^abcLaine, S.; Dey, L.; Valtonen, M.; Gopakumar, A.; Zola, S.; Komossa, S.; Kidger, M.; Pihajoki, P.; Gómez, J.L.; Caton, D.; Ciprini, S.; Drozdz, M.; Gazeas, K.; Godunova, V.; Haque, S.; Hildebrandt, F.; Hudec, R.; Jermak, H.; Kong, A.K.H.; Lehto, H.; Liakos, A.; Matsumoto, K.; Mugrauer, M.; Pursimo, T.; Reichart, D.E.; Simon, A.; Siwak, M.; Sonbas, E. (2020)."Spitzer Observations of the Predicted Eddington Flare from Blazar OJ 287"(PDF).The Astrophysical Journal.894(1): L1.arXiv:2004.13392.Bibcode:2020ApJ...894L...1L.doi:10.3847/2041-8213/ab79a4.S2CID216562421.
  5. ^ab"Spitzer Telescope Reveals the Precise Timing of a Black Hole Dance".JPL.NASA.gov.Jet Propulsion Laboratory. 28 April 2020.Retrieved2020-05-03.
  6. ^ab"Weighing OJ 287 and the project MOMO".mpifr-bonn.mpg.de.Retrieved2023-02-27.
  7. ^Fish, Vincent; Akiyama, Kazunori; Bouman, Katherine; Chael, Andrew; Johnson, Michael; Doeleman, Sheperd; Blackburn, Lindy; Wardle, John; Freeman, William; the Event Horizon Telescope Collaboration (2016-10-27)."Observing—and Imaging—Active Galactic Nuclei with the Event Horizon Telescope".Galaxies.4(4): 54.arXiv:1607.03034.Bibcode:2016Galax...4...54F.doi:10.3390/galaxies4040054.ISSN2075-4434.
  8. ^Shi, Weizhao; Liu, Xiang; Song, Huagang (2007). "A new model for the periodic outbursts of the BL Lac object OJ287".Astrophysics and Space Science.310(1–2): 59–63.Bibcode:2007Ap&SS.310...59S.doi:10.1007/s10509-007-9413-z.S2CID121149840.
  9. ^Valtonen, M. J.; Nilsson, K.; Sillanpää, A.; et al. (2006)."The 2005 November Outburst in OJ 287 and the Binary Black Hole Model".The Astrophysical Journal.643(1): L9–L12.Bibcode:2006ApJ...643L...9V.doi:10.1086/505039.
  10. ^Valtonen, M. J.;Mikkola, S.;Merritt, D.;et al. (February 2010). "Measuring the Spin of the Primary Black Hole in OJ287".The Astrophysical Journal.709(1): 725–732.arXiv:0912.1209.Bibcode:2010ApJ...709..725V.doi:10.1088/0004-637X/709/2/725.S2CID119276181.
  11. ^Shiga, David (10 January 2008)."Biggest black hole in the cosmos discovered".NewScientist news service.
  12. ^Valtonen, M. J.; Lehto, H. J.; Sillanpaa, A.; et al. (2006)."Predicting the Next Outbursts of OJ 287 in 2006–2010".The Astrophysical Journal.646(1): 36–48.Bibcode:2006ApJ...646...36V.doi:10.1086/504884..
  13. ^Dey, L.; Gopakumar, A.; Valtonen, M.; Zola, S.; Susobhanan, A.; Hudec, R.; Pihajoki, P.; Pursimo, T.; Berdyugin, A.; Piirola, V.; Ciprini, S.; Nilsson, K.; Jermak, H.; Kidger, M.; Komossa, S. (2019)."The Unique Blazar OJ 287 and Its Massive Binary Black Hole Central Engine".Universe.5(5): 108.arXiv:1905.02689.Bibcode:2019Univ....5..108D.doi:10.3390/universe5050108.S2CID146808185.

External links[edit]


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