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Rapid quasi-periodic oscillations in the relativistic jet of BL Lacertae.
Jorstad, S G; Marscher, A P; Raiteri, C M; Villata, M; Weaver, Z R; Zhang, H; Dong, L; Gómez, J L; Perel, M V; Savchenko, S S; Larionov, V M; Carosati, D; Chen, W P; Kurtanidze, O M; Marchini, A; Matsumoto, K; Mortari, F; Aceti, P; Acosta-Pulido, J A; Andreeva, T; Apolonio, G; Arena, C; Arkharov, A; Bachev, R; Banfi, M; Bonnoli, G; Borman, G A; Bozhilov, V; Carnerero, M I; Damljanovic, G; Ehgamberdiev, S A; Elsässer, D; Frasca, A; Gabellini, D; Grishina, T S; Gupta, A C; Hagen-Thorn, V A; Hallum, M K; Hart, M; Hasuda, K; Hemrich, F; Hsiao, H Y; Ibryamov, S; Irsmambetova, T R; Ivanov, D V; Joner, M D; Kimeridze, G N; Klimanov, S A; Knött, J; Kopatskaya, E N.
Affiliation
  • Jorstad SG; Institute for Astrophysical Research, Boston University, Boston, MA, USA. jorstad@bu.edu.
  • Marscher AP; Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia. jorstad@bu.edu.
  • Raiteri CM; Institute for Astrophysical Research, Boston University, Boston, MA, USA.
  • Villata M; INAF, Osservatorio Astrofisico di Torino, Torino, Italy.
  • Weaver ZR; INAF, Osservatorio Astrofisico di Torino, Torino, Italy.
  • Zhang H; Institute for Astrophysical Research, Boston University, Boston, MA, USA.
  • Dong L; NASA Postdoctoral Program Fellow, Greenbelt, MD, USA.
  • Gómez JL; NASA Goddard Space Flight Center, Greenbelt, MD, USA.
  • Perel MV; Department of Physics, Purdue University, West Lafayette, IN, USA.
  • Savchenko SS; Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain.
  • Larionov VM; St. Petersburg State University, St. Petersburg, Russia.
  • Carosati D; Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia.
  • Chen WP; Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz, Russia.
  • Kurtanidze OM; Pulkovo Observatory, St. Petersburg, Russia.
  • Marchini A; Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia.
  • Matsumoto K; Pulkovo Observatory, St. Petersburg, Russia.
  • Mortari F; EPT Observatories, Tijarafe, La Palma, Spain.
  • Aceti P; INAF, TNG Fundación Galileo Galilei, La Palma, Spain.
  • Acosta-Pulido JA; Graduate Institute of Astronomy, National Central University, Taoyuan, Taiwan.
  • Andreeva T; Abastumani Observatory, Mt. Kanobili, Abastumani, Georgia.
  • Apolonio G; Engelhardt Astronomical Observatory, Kazan Federal University, Tatarstan, Russia.
  • Arena C; Zentrum für Astronomie der Universität Heidelberg, Landessternwarte, Heidelberg, Germany.
  • Arkharov A; Astronomical Observatory, Department of Physical Sciences, Earth and Environment, University of Siena, Siena, Italy.
  • Bachev R; Astronomical Institute, Osaka Kyoiku University, Kashiwara, Japan.
  • Banfi M; Hypatia Observatory, Rimini, Italy.
  • Bonnoli G; Osservatorio Astronomico Città di Seveso, Seveso, Italy.
  • Borman GA; Department of Aerospace Science and Technology, Politecnico di Milano, Milano, Italy.
  • Bozhilov V; Instituto de Astrofísica de Canarias and Dpto. de Astrofísica, Universidad de La Laguna, Tenerife, Spain.
  • Carnerero MI; Institute of Applied Astronomy, Russian Academy of Sciences, St. Petersburg, Russia.
  • Damljanovic G; Department of Physics and Astronomy, Brigham Young University, Provo, UT, USA.
  • Ehgamberdiev SA; Gruppo Astrofili Catanesi (GAC), Catania, Italy.
  • Elsässer D; Pulkovo Observatory, St. Petersburg, Russia.
  • Frasca A; Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Sofia, Bulgaria.
  • Gabellini D; Osservatorio Astronomico Città di Seveso, Seveso, Italy.
  • Grishina TS; Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain.
  • Gupta AC; Astronomical Observatory, Department of Physical Sciences, Earth and Environment, University of Siena, Siena, Italy.
  • Hagen-Thorn VA; INAF-Osservatorio Astronomico di Brera, Merate, Italy.
  • Hallum MK; Crimean Astrophysical Observatory RAS, Bakhchisaray, Crimea.
  • Hart M; Department of Astronomy, Faculty of Physics, University of Sofia, Sofia, Bulgaria.
  • Hasuda K; INAF, Osservatorio Astrofisico di Torino, Torino, Italy.
  • Hemrich F; Astronomical Observatory Belgrade, Belgrade, Serbia.
  • Hsiao HY; Ulugh Beg Astronomical Institute, Tashkent, Uzbekistan.
  • Ibryamov S; National University of Uzbekistan, Tashkent, Uzbekistan.
  • Irsmambetova TR; Hans-Haffner-Sternwarte, Naturwissenschaftliches Labor für Schüler am FKG, Würzburg, Germany.
  • Ivanov DV; Department of Physics, TU Dortmund University, Dortmund, Germany.
  • Joner MD; INAF-Osservatorio Astrofisico di Catania, Catania, Italy.
  • Kimeridze GN; Hypatia Observatory, Rimini, Italy.
  • Klimanov SA; Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia.
  • Knött J; Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital, India.
  • Kopatskaya EN; Astronomical Institute, St. Petersburg State University, St. Petersburg, Russia.
Nature ; 609(7926): 265-268, 2022 09.
Article in En | MEDLINE | ID: mdl-36071186
ABSTRACT
Blazars are active galactic nuclei (AGN) with relativistic jets whose non-thermal radiation is extremely variable on various timescales1-3. This variability seems mostly random, although some quasi-periodic oscillations (QPOs), implying systematic processes, have been reported in blazars and other AGN. QPOs with timescales of days or hours are especially rare4 in AGN and their nature is highly debated, explained by emitting plasma moving helically inside the jet5, plasma instabilities6,7 or orbital motion in an accretion disc7,8. Here we report results of intense optical and γ-ray flux monitoring of BL Lacertae (BL Lac) during a dramatic outburst in 2020 (ref. 9). BL Lac, the prototype of a subclass of blazars10, is powered by a 1.7 × 108 MSun (ref. 11) black hole in an elliptical galaxy (distance = 313 megaparsecs (ref. 12)). Our observations show QPOs of optical flux and linear polarization, and γ-ray flux, with cycles as short as approximately 13 h during the highest state of the outburst. The QPO properties match the expectations of current-driven kink instabilities6 near a recollimation shock about 5 parsecs (pc) from the black hole in the wake of an apparent superluminal feature moving down the jet. Such a kink is apparent in a microwave Very Long Baseline Array (VLBA) image.
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Full text: 1 Collection: 01-internacional Database: MEDLINE Language: En Journal: Nature Year: 2022 Type: Article Affiliation country: United States
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Full text: 1 Collection: 01-internacional Database: MEDLINE Language: En Journal: Nature Year: 2022 Type: Article Affiliation country: United States