Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/26764
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Nava, Lara | en_US |
dc.contributor.author | Benyamin, David | en_US |
dc.contributor.author | Piran, Tsvi | en_US |
dc.contributor.author | Shaviv, Nir J. | en_US |
dc.date.accessioned | 2020-08-21T16:08:20Z | - |
dc.date.available | 2020-08-21T16:08:20Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26764 | - |
dc.description.abstract | Most of the diffuse Galactic GeV γ-ray emission is produced via collisions of cosmic ray (CR) protons with ISM protons. As such the observed spectra of the γ-rays and the CRs should be strongly linked. Recent observations of Fermi-LAT exhibit a hardening of the γ-ray spectrum at around a hundred GeV, between the Sagittarius and Carina tangents, and a further hardening at a few degrees above and below the Galactic plane. However, standard CR propagation models that assume a time-independent source distribution and a location-independent diffusion cannot give rise to a spatially dependent CR (and hence γ-ray) spectral slopes. Here, we consider a dynamic spiral arm model in which the distribution of CR sources is concentrated in the (dynamic) spiral arms, and we study the effects of this model on the π<SUP>0</SUP>-decay-produced γ-ray spectra. Within this model, near the Galactic arms the observed γ-ray spectral slope is not trivially related to the CR injection spectrum and energy dependence of the diffusion coefficient. We find unique signatures that agree with the Fermi-LAT observations. This model also provides a physical explanation for the difference between the local CR spectral slope and the CR slope inferred from the average γ-ray spectrum. | en_US |
dc.language.iso | eng | en_US |
dc.title | Reconciling the diffuse Galactic γ-ray and the cosmic ray spectra | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stw3346 | en_US |
dc.identifier.scopus | 2-s2.0-85018282785 | en_US |
dc.identifier.isi | 000398418600086 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/466/3/3674/2736302 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 466 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 3674 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 4 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | USA | en_US |
dc.contributor.country | ISR | 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 | 2017MNRAS.466.3674N | en_US |
dc.relation.fund | FP7 | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::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.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.orcid | 0000-0001-5960-0455 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
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