Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/28540
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Kapanadze, B. | en_US |
dc.contributor.author | Dorner, D. | en_US |
dc.contributor.author | ROMANO, Patrizia | en_US |
dc.contributor.author | VERCELLONE, STEFANO | en_US |
dc.contributor.author | Kapanadze, S. | en_US |
dc.contributor.author | Tabagari, L. | en_US |
dc.date.accessioned | 2020-11-25T12:24:00Z | - |
dc.date.available | 2020-11-25T12:24:00Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/28540 | - |
dc.description.abstract | We present the results of the Swift observations of the nearby BL Lac object Mrk 421 during 2013 November-2015 June. The source exhibited a strong long-term variability in the 0.3-10 keV band, with a maximum-to-minimum flux ratio of 13, and underwent X-ray flares by a factor of 1.8-5.2 on timescales of a few weeks or shorter. The source showed 48 instances of intraday flux variability in this period, which sometimes was observed within the 1 ks observational run. It was characterized by fractional amplitudes of 1.5(0.3)%-38.6(0.4)% and flux doubling/halving times of 2.6-20.1 hr. The X-ray flux showed a lack of correlation with the TeV flux on some occasions (strong TeV flares were not accompanied by comparable X-ray activity and vice versa), indicating that the high-energy emission in Mrk 421 was generated from an emission region more complex than a single zone. The best fits of the 0.3-10 keV spectra were mainly obtained using the log-parabola model, showing a strong spectral variability that generally followed a “harder-when-brighter” trend. The position of the synchrotron spectral energy distribution peak showed an extreme range from a few eV to ∼10 keV that happens rarely in blazars. | en_US |
dc.language.iso | eng | en_US |
dc.title | Mrk 421 after the Giant X-Ray Outburst in 2013 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/aa8ea6 | en_US |
dc.identifier.scopus | 2-s2.0-85032807413 | en_US |
dc.identifier.isi | 000413339200003 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/aa8ea6 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 848 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.numberofpages | 26 | en_US |
dc.relation.article | 103 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 6 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | GEO | en_US |
dc.contributor.country | GEO | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2017ApJ...848..103K | 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 | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.orcid | 0000-0003-0258-7469 | - |
crisitem.author.orcid | 0000-0003-1163-1396 | - |
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