We describe a scenario to explain blazar periodicities with time-scales of similar to few years. The scenario is based on a binary supermassive black hole (SMBH) system in which one of the two SMBHs carries a jet. We discuss the various mechanisms that can cause the jet to precess and produce corkscrew patterns through space with a scale of similar to few pc. It turns out that the dominant mechanism responsible for the precession is simply the imprint of the jet-carrying SMBH orbital speed on the jet. Gravitational deflection and Lense-Thirring precession (due to the gravitational field of the other SMBH) are second-order effects. We complement the scenario with a kinematical jet model which is inspired to the spine-sheath structure observed in M87. One of the main advantages of such a structure is that it allows the peak of the synchrotron emission to scale with frequency according to nu F alpha nu(xi) as the viewing angle is changed, where. is not necessarily 3 or 4 as in the case of jets with uniform velocity, but can be xi similar to 1. Finally, we apply the model to the source PG1553+113, which has been recently claimed to show a T-obs = (2.18 +/- 0.08) yr periodicity. We are able to reproduce the optical and gamma-ray light curves and multiple synchrotron spectra simultaneously. We also give estimates of the source mass and size.

A model for periodic blazars

Sormani M
;
2017-01-01

Abstract

We describe a scenario to explain blazar periodicities with time-scales of similar to few years. The scenario is based on a binary supermassive black hole (SMBH) system in which one of the two SMBHs carries a jet. We discuss the various mechanisms that can cause the jet to precess and produce corkscrew patterns through space with a scale of similar to few pc. It turns out that the dominant mechanism responsible for the precession is simply the imprint of the jet-carrying SMBH orbital speed on the jet. Gravitational deflection and Lense-Thirring precession (due to the gravitational field of the other SMBH) are second-order effects. We complement the scenario with a kinematical jet model which is inspired to the spine-sheath structure observed in M87. One of the main advantages of such a structure is that it allows the peak of the synchrotron emission to scale with frequency according to nu F alpha nu(xi) as the viewing angle is changed, where. is not necessarily 3 or 4 as in the case of jets with uniform velocity, but can be xi similar to 1. Finally, we apply the model to the source PG1553+113, which has been recently claimed to show a T-obs = (2.18 +/- 0.08) yr periodicity. We are able to reproduce the optical and gamma-ray light curves and multiple synchrotron spectra simultaneously. We also give estimates of the source mass and size.
2017
2016
BL Lacertae objects: general – BL Lacertae objects: individual: PG1553+113 – galaxies: jets
Sobacchi, E; Sormani, M; Stamerra, A
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11383/2170731
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