Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/23955
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Beniamini, Paz | en_US |
dc.contributor.author | Nava, Lara | en_US |
dc.contributor.author | Barniol Duran, Rodolfo | en_US |
dc.contributor.author | Piran, Tsvi | en_US |
dc.date.accessioned | 2020-04-09T11:48:37Z | - |
dc.date.available | 2020-04-09T11:48:37Z | - |
dc.date.issued | 2015 | en_US |
dc.identifier.issn | 1824-8039 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/23955 | - |
dc.description.abstract | We examine GRBs with both Fermi-LAT and X-ray afterglow data. Assuming that the 100MeV (LAT) emission is radiation from cooled electrons accelerated by external shocks, we show that the kinetic energy of the blast wave estimated from the 100MeV flux is 50 times larger than the one estimated from the X-ray flux. This can be explained if either: i) electrons radiating at X-rays are significantly cooled by SSC (suppressing the synchrotron flux above the cooling frequency) or ii) if the X-ray emitting electrons, unlike those emitting at 100MeV energies, are in the slow cooling regime. In both cases the X-ray flux is no longer an immediate proxy of the blast wave kinetic energy. We model the LAT, X-ray and optical data and show that in general these possibilities are consistent with the data, and explain the apparent disagreement between X-ray and LAT observations. All possible solutions require weak magnetic fields: $10^{-6}< \epsilon_B < 10^{-3}$ (where $\epsilon_B$ is the fraction of shocked plasma energy in magnetic fields). Using the LAT emission as a proxy for the blast wave kinetic energy we find that the derived prompt efficiencies are of order 15%. This is considerably lower compared with previous estimates (87% and higher for the same bursts). This provides at least a partial solution to the "prompt high efficiency paradox" | en_US |
dc.language.iso | eng | en_US |
dc.title | Shedding light on the prompt high efficiency paradox - self consistent modeling of GRB afterglows | en_US |
dc.type | Conference paper | - |
dc.identifier.doi | 10.22323/1.233.0064 | en_US |
dc.identifier.url | https://pos.sissa.it/233/064/ | en_US |
dc.relation.medium | ELETTRONICO | en_US |
dc.relation.volume | 233 | en_US |
dc.relation.numberofpages | 6 | en_US |
dc.type.referee | REF_0 | en_US |
dc.description.numberofauthors | 4 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.contributor.country | ISR | en_US |
dc.relation.alleditors | Caraveo, Patrizia; D’Avanzo, Paolo; Gehrels, Neil; Tagliaferri, Gianpiero | en_US |
dc.relation.ispartofbook | Swift: 10 Years of Discovery (SWIFT 10) | en_US |
dc.type.invited | no | en_US |
dc.relation.conferencename | Swift: 10 Years of Discovery | en_US |
dc.relation.conferenceplace | La Sapienza University, Rome, Italy | en_US |
dc.relation.conferencedate | 2-5 December 2014 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | POS PROCEEDINGS OF SCIENCE | en_US |
dc.type.miur | 273 Contributo in Atti di convegno | - |
dc.identifier.adsbibcode | 2015arXiv150303368B | en_US |
dc.relation.ercsector | Scienze Fisiche Settori ERC (ERC) di riferimento::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation | 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 | Conference paper | - |
crisitem.journal.journalissn | 1824-8039 | - |
crisitem.journal.ance | E188909 | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.orcid | 0000-0001-5960-0455 | - |
È visualizzato nelle collezioni: | 3.01 Contributi in Atti di convegno |
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