Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/25877
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Kapanadze, B. | en_US |
dc.contributor.author | Dorner, D. | en_US |
dc.contributor.author | VERCELLONE, STEFANO | en_US |
dc.contributor.author | ROMANO, Patrizia | en_US |
dc.contributor.author | Kapanadze, S. | en_US |
dc.contributor.author | Mdzinarishvili, T. | en_US |
dc.date.accessioned | 2020-06-01T16:25:35Z | - |
dc.date.available | 2020-06-01T16:25:35Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/25877 | - |
dc.description.abstract | We present an X-ray flaring activity of 1ES 1959+650 in 2015 August-2016 January, which was the most powerful and prolonged during the 10.75 yr period since the start of its monitoring with X-ray Telescope onboard Swift. A new highest historical 0.3-10 keV count rate was recorded three times that makes this object the third BL Lacertae source exceeding the level of 20 counts s<SUP>-1</SUP>. Along with the overall variability by a factor of 5.7, this epoch was characterized by fast X-ray flares by a factor of 2.0-3.1, accompanied with an extreme spectral variability. The source also shows a simultaneous flaring activity in the optical - UV and 0.3-100 GeV bands, although a fast γ-ray flare without significant optical - X-ray counterparts is also found. In contrast to the X-ray flares in the previous years, the stochastic acceleration seems be less important for the electrons responsible for producing X-ray emission during this flare that challenges the earlier suggestion that the electrons in the jets of TeV-detected BL Lacertae objects should undergo an efficient stochastic acceleration resulting in a lower X-ray spectral curvature. | en_US |
dc.language.iso | eng | en_US |
dc.title | A recent strong X-ray flaring activity of 1ES 1959+650 with possibly less efficient stochastic acceleration | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnrasl/slw054 | en_US |
dc.identifier.scopus | 2-s2.0-84982286514 | en_US |
dc.identifier.isi | 000383269900006 | en_US |
dc.identifier.url | https://academic.oup.com/mnrasl/article/461/1/L26/2589500 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 461 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | L26 | en_US |
dc.relation.lastpage | L31 | en_US |
dc.relation.numberofpages | 6 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | 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 | 2016MNRAS.461L..26K | 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.cerifentitytype | Publications | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.orcid | 0000-0003-1163-1396 | - |
crisitem.author.orcid | 0000-0003-0258-7469 | - |
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