Bibcode
Raiteri, C. M.; Villata, M.; Acosta-Pulido, J. A.; Agudo, I.; Arkharov, A. A.; Bachev, R.; Baida, G. V.; Benítez, E.; Borman, G. A.; Boschin, W.; Bozhilov, V.; Butuzova, M. S.; Calcidese, P.; Carnerero, M. I.; Carosati, D.; Casadio, C.; Castro-Segura, N.; Chen, W.-P.; Damljanovic, G.; D’Ammando, F.; di Paola, A.; Echevarría, J.; Efimova, N. V.; Ehgamberdiev, Sh. A.; Espinosa, C.; Fuentes, A.; Giunta, A.; Gómez, J. L.; Grishina, T. S.; Gurwell, M. A.; Hiriart, D.; Jermak, H.; Jordan, B.; Jorstad, S. G.; Joshi, M.; Kopatskaya, E. N.; Kuratov, K.; Kurtanidze, O. M.; Kurtanidze, S. O.; Lähteenmäki, A.; Larionov, V. M.; Larionova, E. G.; Larionova, L. V.; Lázaro, C.; Lin, C. S.; Malmrose, M. P.; Marscher, A. P.; Matsumoto, K.; McBreen, B.; Michel, R.; Mihov, B.; Minev, M.; Mirzaqulov, D. O.; Mokrushina, A. A.; Molina, S. N.; Moody, J. W.; Morozova, D. A.; Nazarov, S. V.; Nikolashvili, M. G.; Ohlert, J. M.; Okhmat, D. N.; Ovcharov, E.; Pinna, F.; Polakis, T. A.; Protasio, C.; Pursimo, T.; Redondo-Lorenzo, F. J.; Rizzi, N.; Rodriguez-Coira, G.; Sadakane, K.; Sadun, A. C.; Samal, M. R.; Savchenko, S. S.; Semkov, E.; Skiff, B. A.; Slavcheva-Mihova, L.; Smith, P. S.; Steele, I. A.; Strigachev, A.; Tammi, J.; Thum, C.; Tornikoski, M.; Troitskaya, Yu. V.; Troitsky, I. S.; Vasilyev, A. A.; Vince, O.
Referencia bibliográfica
Nature, Volume 552, Issue 7685, pp. 374-377 (2017).
Fecha de publicación:
12
2017
Revista
Número de citas
132
Número de citas referidas
124
Descripción
Blazars are active galactic nuclei, which are powerful sources of
radiation whose central engine is located in the core of the host
galaxy. Blazar emission is dominated by non-thermal radiation from a jet
that moves relativistically towards us, and therefore undergoes Doppler
beaming. This beaming causes flux enhancement and contraction of the
variability timescales, so that most blazars appear as luminous sources
characterized by noticeable and fast changes in brightness at all
frequencies. The mechanism that produces this unpredictable variability
is under debate, but proposed mechanisms include injection, acceleration
and cooling of particles, with possible intervention of shock waves or
turbulence. Changes in the viewing angle of the observed emitting knots
or jet regions have also been suggested as an explanation of flaring
events and can also explain specific properties of blazar emission, such
as intra-day variability, quasi-periodicity and the delay of radio flux
variations relative to optical changes. Such a geometric interpretation,
however, is not universally accepted because alternative explanations
based on changes in physical conditions—such as the size and speed
of the emitting zone, the magnetic field, the number of emitting
particles and their energy distribution—can explain snapshots of
the spectral behaviour of blazars in many cases. Here we report the
results of optical-to-radio-wavelength monitoring of the blazar CTA 102
and show that the observed long-term trends of the flux and spectral
variability are best explained by an inhomogeneous, curved jet that
undergoes changes in orientation over time. We propose that
magnetohydrodynamic instabilities or rotation of the twisted jet cause
different jet regions to change their orientation and hence their
relative Doppler factors. In particular, the extreme optical outburst of
2016–2017 (brightness increase of six magnitudes) occurred when
the corresponding emitting region had a small viewing angle. The
agreement between observations and theoretical predictions can be seen
as further validation of the relativistic beaming theory.
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