Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/28414
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 | Hughes, P. | en_US |
dc.contributor.author | Aller, M. | en_US |
dc.contributor.author | Aller, H. | en_US |
dc.contributor.author | Reynolds, M. | en_US |
dc.contributor.author | Tabagari, L. | en_US |
dc.date.accessioned | 2020-11-18T12:38:37Z | - |
dc.date.available | 2020-11-18T12:38:37Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0067-0049 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/28414 | - |
dc.description.abstract | We present the detailed timing and spectral results obtained during the Swift observations of the TeV-detected blazar 1ES 1959+650 in 2016 August-2017 November. The source continued its trend of gradually enhancing X-ray flaring activity in the 0.3-10 keV energy range, starting in 2015 August, and a new highest historical brightness state was recorded twice. A long-term high state was superimposed by both weak and strong flares, and we detected 32 instances of intraday X-ray flux variability, including several occasions of extremely fast fluctuations with fractional amplitudes of 5.4%-7.5% within 1 ks exposures. The 0.3-10 keV spectra generally showed a best fit with the log-parabolic model, yielding a very wide range of the curvature parameter b and the photon index at 1 keV. The position of the synchrotron SED peak E <SUB>p</SUB> showed an extreme variability on various timescales between energies less than 0.1 keV and 7.7 ± 0.7 keV, with 25% of the spectra peaking at hard X-rays. In 2017 May-November, the source mostly showed lower spectral curvature and an anticorrelation b-E <SUB>p</SUB>, expected in the case of efficient stochastic acceleration of X-ray-emitting electrons. The 0.3-100 GeV and optical-UV fluxes also attained their highest historical values in this period, although the latter showed an anticorrelation with the 0.3-10 keV emission, which is explained by the stochastic acceleration of electrons with a narrow initial energy distribution, having an average energy significantly higher than the equilibrium energy. | en_US |
dc.language.iso | eng | en_US |
dc.title | Strong X-Ray and Multiwavelength Flaring Activity for 1ES 1959+650, 2016 August-2017 November | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4365/aad8b5 | en_US |
dc.identifier.scopus | 2-s2.0-85054761181 | en_US |
dc.identifier.isi | 000445823200006 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4365/aad8b5 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 238 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 13 | en_US |
dc.relation.numberofpages | 23 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2018ApJS..238...13K | 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. Brera | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.orcid | 0000-0003-1163-1396 | - |
crisitem.author.orcid | 0000-0003-0258-7469 | - |
crisitem.journal.journalissn | 0067-0049 | - |
crisitem.journal.ance | E016254 | - |
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Kapanadze_2018_ApJS_238_13.pdf | Pdf editoriale | 3.14 MB | Adobe PDF | Visualizza/apri |
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