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Catching the radio flare in CTA 102

Christian M. FrommMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, GermanyE. RosDepartament d’Astronomia i Astrofísica, Universitat de València, Dr. Moliner 50, 46100 Burjassot, València, SpainM. PeruchoDepartament d’Astronomia i Astrofísica, Universitat de València, Dr. Moliner 50, 46100 Burjassot, València, SpainT. SavolainenMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, GermanyP. MimicaDepartament d’Astronomia i Astrofísica, Universitat de València, Dr. Moliner 50, 46100 Burjassot, València, SpainM. KadlerInstitut für Theoretische Physik und Astrophysik, Universität Würzburg, Am Hubland, 97074 Würzburg, GermanyA. P. LobanovMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, GermanyJ. A. ZensusMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany

2013en

ABI

Annotatsiya

Context. The temporal and spatial spectral evolution of the jets of active galactic nuclei (AGN) can be studied with multi-frequency, multi-epoch very-long-baseline-interferometry (VLBI) observations. The combination of both morphological (kinematical) and spectral parameters can be used to derive source-intrinsic physical properties, such as the magnetic field and the nonthermal particle density. Such a study is of special interest during the high states of activity in AGNs, since VLBI observations can provide estimates of the location of the flaring site. Furthermore, we can trace the temporal variations in the source-intrinsic parameters during the flare, which may reflect the interaction between the underlying plasma and a traveling shock wave. The source CTA 102 exhibited such a radio flare around 2006.

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DOI: 10.1051/0004-6361/201321784

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