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dc.contributor.author
Acharya, B. S.  
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Aramo, C.  
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Babic, A.  
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Barrio, J. A.  
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Baushev, A.  
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Becker Tjus, J.  
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Berge, D.  
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Bohacova, M.  
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Bonardi, A.  
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Brown, A.  
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Bugaev, V.  
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Bulik, T.  
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Burton, M.  
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Busetto, G.  
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Caraveo, P.  
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Carosi, R.  
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Carr, J.  
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Chadwick, P.  
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Chudoba, J.  
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Conforti, V.  
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Connaughton, V.  
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Contreras, J. L.  
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Cotter, G.  
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Dazzi, F.  
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De Franco, A.  
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de la Calle, I.  
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de los Reyes Lopez, R.  
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De Lotto, B.  
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Garcia, Beatriz Elena  
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Rovero, Adrian Carlos  
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The Cta Consortium  
dc.date.available
2017-06-06T18:01:15Z  
dc.date.issued
2015-03  
dc.identifier.citation
Acharya, B. S.; Aramo, C.; Babic, A.; Barrio, J. A.; Baushev, A.; et al.; The Cherenkov Telescope Array potential for the study of young supernova remnants; Elsevier Science; Astroparticle Physics; 62; 3-2015; 152-164  
dc.identifier.issn
0927-6505  
dc.identifier.uri
http://hdl.handle.net/11336/17573  
dc.description.abstract
Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000 years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models.  
dc.format
application/pdf  
dc.language.iso
eng  
dc.publisher
Elsevier Science  
dc.rights
info:eu-repo/semantics/openAccess  
dc.rights.uri
https://creativecommons.org/licenses/by-nc-nd/2.5/ar/  
dc.subject
Acceleration of Particles  
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Gamma Rays  
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Supernova Remnants  
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Astronomía  
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Ciencias Físicas  
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CIENCIAS NATURALES Y EXACTAS  
dc.title
The Cherenkov Telescope Array potential for the study of young supernova remnants  
dc.type
info:eu-repo/semantics/article  
dc.type
info:ar-repo/semantics/artículo  
dc.type
info:eu-repo/semantics/publishedVersion  
dc.date.updated
2017-06-01T16:45:46Z  
dc.journal.volume
62  
dc.journal.pagination
152-164  
dc.journal.pais
Países Bajos  
dc.journal.ciudad
Amsterdam  
dc.description.fil
Fil: Acharya, B. S.. Tata Institute of Fundamental Research; India  
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Fil: Aramo, C.. INFN; Italia  
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Fil: Babic, A.. Rudjer Boskovic Institute; Croacia  
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Fil: Barrio, J. A.. Universidad Complutense de Madrid; España  
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Fil: Baushev, A.. Universität Potsdam; Alemania  
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Fil: Becker Tjus, J.. Ruhr-universität Bochum; Alemania  
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Fil: Berge, D.. University of Amsterdam; Países Bajos  
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Fil: Bohacova, M.. Institute of Physics of the Academy of Sciences of the Czech Republic; República Checa  
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Fil: Bonardi, A.. Universität Tübingen; Alemania  
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Fil: Brown, A.. Durham University; Reino Unido  
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Fil: Bugaev, V.. Washington University; Estados Unidos  
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Fil: Bulik, T.. University of Warsaw; Polonia  
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Fil: Burton, M.. University Of New South Wales; Australia  
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Fil: Busetto, G.. Universitá degli Studi di Padova; Italia  
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Fil: Caraveo, P.. Istituto di Astrofisica Spaziale e Fisica Cosmica; Italia  
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Fil: Carosi, R.. INFN; Italia  
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Fil: Carr, J.. Aix-Marseille Université; Francia  
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Fil: Chadwick, P.. Durham University; Reino Unido  
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Fil: Chudoba, J.. Institute of Physics of the Academy of Sciences of the Czech Republic; República Checa  
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Fil: Conforti, V.. Istituto di Astrofisica Spaziale e Fisica Cosmica; Italia  
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Fil: Connaughton, V.. University of Alabama; Estados Unidos  
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Fil: Contreras, J. L.. Universidad Complutense de Madrid; España  
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Fil: Cotter, G.. University of Oxford; Reino Unido  
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Fil: Dazzi, F.. Universitá degli Studi di Padova; Italia  
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Fil: De Franco, A.. t University of Oxford; Reino Unido  
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Fil: de la Calle, I.. Universidad Complutense de Madrid; España  
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Fil: de los Reyes Lopez, R.. Max-Planck-Institut für Kernphysik; Alemania  
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Fil: De Lotto, B.. University of Udine; Italia  
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Fil: Garcia, Beatriz Elena. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Parque Centenario. Instituto de Tecnologías en Detección y Astropartículas. Subsede del Instituto de Tecnologías en Detección y Astropartículas Mendoza; Argentina  
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Fil: Rovero, Adrian Carlos. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina  
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Fil: The Cta Consortium.  
dc.journal.title
Astroparticle Physics  
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1016/j.astropartphys.2014.08.005  
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info:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S0927650514001297