FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W1971748324> ?p ?o ?g. }

• W1971748324 endingPage "968" @default.
• W1971748324 startingPage "958" @default.
• W1971748324 abstract "X-ray observations of Seyfert 1 galaxies offer the unique possibility of observing spectral variability on time-scales comparable to the dynamical time of the inner accretion flow. They typically show highly variable light curves, on a wide range of time-scales, with power density spectra characterized by ‘red noise’ and a break at low frequencies. On the other hand, time-resolved spectral analyses have established that spectral variability on the shortest time-scales is important in all these sources, with the spectra getting softer at high fluxes (in the band, typically), while the reflection component and the iron line often exhibit a complex behaviour. Here we present a model that is able to explain a number of the above mentioned properties, in terms of magnetic flares shining above a standard accretion disc producing the X-ray spectrum via inverse Compton scattering of soft photons (both intrinsic and reprocessed thermal emission from the accretion disc and locally produced synchrotron radiation). We show that the fundamental heating event, likely caused by magnetic reconnection, must be compact, with typical size comparable to the accretion disc thickness, and must be triggered at a height at least an order of magnitude larger than its size. The fundamental property of our ‘thundercloud’ model is that the spatial and temporal distributions of flares are not random: the heating of the corona proceeds in correlated trains of events in an avalanche fashion. The amplitude of the avalanches obeys a power-law distribution and determines the size of the active regions where the spectrum is produced. As a result of the feedback effect of the X-ray radiation reprocessed in the disc, larger active regions produce softer spectra. With our model we simulate X-ray light curves that reproduce the main observational properties of the power density spectra and of the X-ray continuum short-term variability of Seyfert 1 galaxies. By comparing them with observations of MGC–6-30-15, we are able to infer that the accretion disc corona in this source must have a large optical depth and small average covering fraction." @default.
• W1971748324 created "2016-06-24" @default.
• W1971748324 creator A5021019655 @default.
• W1971748324 creator A5024983697 @default.
• W1971748324 date "2001-12-01" @default.
• W1971748324 modified "2023-10-18" @default.
• W1971748324 title "Thunderclouds and accretion discs: a model for the spectral and temporal variability of Seyfert 1 galaxies" @default.
• W1971748324 cites W1601784226 @default.
• W1971748324 cites W1844333606 @default.
• W1971748324 cites W1978505636 @default.
• W1971748324 cites W1981214860 @default.
• W1971748324 cites W1982481606 @default.
• W1971748324 cites W1988722437 @default.
• W1971748324 cites W1990386756 @default.
• W1971748324 cites W1990418509 @default.
• W1971748324 cites W1999220943 @default.
• W1971748324 cites W2010920350 @default.
• W1971748324 cites W2017772783 @default.
• W1971748324 cites W2022115999 @default.
• W1971748324 cites W2022937888 @default.
• W1971748324 cites W2025276191 @default.
• W1971748324 cites W2038893224 @default.
• W1971748324 cites W2043503631 @default.
• W1971748324 cites W2044279459 @default.
• W1971748324 cites W2047844795 @default.
• W1971748324 cites W2052685494 @default.
• W1971748324 cites W2052935001 @default.
• W1971748324 cites W2057302115 @default.
• W1971748324 cites W2062381182 @default.
• W1971748324 cites W2067626549 @default.
• W1971748324 cites W2069772990 @default.
• W1971748324 cites W2070202487 @default.
• W1971748324 cites W2075514521 @default.
• W1971748324 cites W2076299185 @default.
• W1971748324 cites W2078719403 @default.
• W1971748324 cites W2080657784 @default.
• W1971748324 cites W2081293134 @default.
• W1971748324 cites W2083439141 @default.
• W1971748324 cites W2083748562 @default.
• W1971748324 cites W2088772258 @default.
• W1971748324 cites W2096220160 @default.
• W1971748324 cites W2101720986 @default.
• W1971748324 cites W2116319976 @default.
• W1971748324 cites W2124186607 @default.
• W1971748324 cites W2138790789 @default.
• W1971748324 cites W2144732404 @default.
• W1971748324 cites W2171203348 @default.
• W1971748324 cites W3099062640 @default.
• W1971748324 cites W3099357603 @default.
• W1971748324 cites W3099861034 @default.
• W1971748324 cites W3100150377 @default.
• W1971748324 cites W3100631579 @default.
• W1971748324 cites W3102848272 @default.
• W1971748324 cites W3103780205 @default.
• W1971748324 cites W3104534720 @default.
• W1971748324 cites W3105371070 @default.
• W1971748324 cites W3121267309 @default.
• W1971748324 cites W3122564296 @default.
• W1971748324 doi "https://doi.org/10.1046/j.1365-8711.2001.04925.x" @default.
• W1971748324 hasPublicationYear "2001" @default.
• W1971748324 type Work @default.
• W1971748324 sameAs 1971748324 @default.
• W1971748324 citedByCount "83" @default.
• W1971748324 countsByYear W19717483242012 @default.
• W1971748324 countsByYear W19717483242013 @default.
• W1971748324 countsByYear W19717483242014 @default.
• W1971748324 countsByYear W19717483242015 @default.
• W1971748324 countsByYear W19717483242016 @default.
• W1971748324 countsByYear W19717483242017 @default.
• W1971748324 countsByYear W19717483242018 @default.
• W1971748324 countsByYear W19717483242020 @default.
• W1971748324 countsByYear W19717483242021 @default.
• W1971748324 countsByYear W19717483242022 @default.
• W1971748324 countsByYear W19717483242023 @default.
• W1971748324 crossrefType "journal-article" @default.
• W1971748324 hasAuthorship W1971748324A5021019655 @default.
• W1971748324 hasAuthorship W1971748324A5024983697 @default.
• W1971748324 hasBestOaLocation W19717483242 @default.
• W1971748324 hasConcept C105795698 @default.
• W1971748324 hasConcept C120665830 @default.
• W1971748324 hasConcept C121332964 @default.
• W1971748324 hasConcept C1276947 @default.
• W1971748324 hasConcept C159317903 @default.
• W1971748324 hasConcept C168110828 @default.
• W1971748324 hasConcept C180205008 @default.
• W1971748324 hasConcept C2776401274 @default.
• W1971748324 hasConcept C2776779350 @default.
• W1971748324 hasConcept C2779900269 @default.
• W1971748324 hasConcept C30475298 @default.
• W1971748324 hasConcept C33923547 @default.
• W1971748324 hasConcept C43481613 @default.
• W1971748324 hasConcept C44870925 @default.
• W1971748324 hasConcept C4839761 @default.
• W1971748324 hasConcept C87355193 @default.
• W1971748324 hasConcept C98444146 @default.
• W1971748324 hasConceptScore W1971748324C105795698 @default.
• W1971748324 hasConceptScore W1971748324C120665830 @default.
• W1971748324 hasConceptScore W1971748324C121332964 @default.

• next