Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/27221
DC Field | Value | Language |
---|---|---|
dc.contributor.author | SOBACCHI, Emanuele | en_US |
dc.contributor.author | Sormani, Mattia C. | en_US |
dc.contributor.author | STAMERRA, Antonio | en_US |
dc.date.accessioned | 2020-09-08T13:24:52Z | - |
dc.date.available | 2020-09-08T13:24:52Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27221 | - |
dc.description.abstract | We describe a scenario to explain blazar periodicities with time-scales of ∼ 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 ∼ 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 νF ∝ ν<SUP>ξ</SUP> as the viewing angle is changed, where ξ is not necessarily 3 or 4 as in the case of jets with uniform velocity, but can be ξ ∼ 1. Finally, we apply the model to the source PG1553+113, which has been recently claimed to show a T<SUB>obs</SUB> = (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. | en_US |
dc.language.iso | eng | en_US |
dc.title | A model for periodic blazars | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stw2684 | en_US |
dc.identifier.scopus | 2-s2.0-85014784986 | en_US |
dc.identifier.isi | 000393782000013 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/465/1/161/2417411 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 465 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 161 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 3 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | GBR | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2017MNRAS.465..161S | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.orcid | 0000-0002-9430-5264 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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tmpQ5AziG.pdf | Pdf editoriale | 1.01 MB | Adobe PDF | View/Open |
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