Acharya, B.S. and Aramo, C. and Babic, A. and Barrio, J.A. and Baushev, A. and Becker Tjus, J. and Berge, D. and Bohacova, M. and Bonardi, A. and Brown, A. and Bugaev, V. and Bulik, T. and Burton, M. and Busetto, G. and Caraveo, P. and Carosi, R. and Carr, J. and Chadwick, P. and Chudoba, J. and Conforti, V. and Connaughton, V. and Contreras, J.L. and Cotter, G. and Dazzi, F. and De Franco, A. and de la Calle, I. and de los Reyes Lopez, R. and De Lotto, B. and De Palma, F. and Di Girolamo, T. and Di Giulio, C. and Di Pierro, F. and Dournaux, J.-L. and Dwarkadas, V. and Ebr, J. and Egberts, K. and Fesquet, M. and Fleischhack, H. and Font, L. and Fontaine, G. and Förster, A. and Fuessling, M. and Garcia, B. and Garcia López, R. and Garczarczyk, M. and Gargano, F. and Garrido, D. and Gaug, M. and Giglietto, N. and Giordano, F. and Giuliani, A. and Godinovic, N. and Gonzalez, M.M. and Grabarczyk, T. and Hassan, T. and Hörandel, J. and Hrabovsky, M. and Hrupec, D. and Humensky, T.B. and Huovelin, J. and Jamrozy, M. and Janecek, P. and Kaaret, P.E. and Katz, U. and Kaufmann, S. and Khélifi, B. and Kluźniak, W. and Kocot, J. and Komin, N. and Kubo, H. and Kushida, J. and Lamanna, G. and Lee, W.H. and Lenain, J.-P. and Lohse, T. and Lombardi, S. and López-Coto, R. and López-Oramas, A. and Lucarelli, F. and Maccarone, M.C. and Maier, G. and Majumdar, P. and Malaguti, G. and Mandat, D. and Mazziotta, M.N. and Meagher, K. and Mirabal, N. and Morselli, A. and Moulin, E. and Niemiec, J. and Nievas, M. and Nishijima, K. and Nosek, D. and Nunio, F. and Ohishi, M. and Ohm, S. and Ong, R.A. and Orito, R. and Otte, N. and Palatka, M. and Pareschi, G. and Pech, M. and Persic, M. and Pohl, M. and Prouza, M. and Quirrenbach, A. and Rainó, S. and Rodriguez Fernandez, G. and Romano, P. and Rovero, A.C. and Rudak, B. and Schovanek, P. and Shayduk, M. and Siejkowski, H. and Sillanpää, A. and Stefanik, S. and Stolarczyk, T. and Szanecki, M. and Szepieniec, T. and Tejedor, L.A. and Telezhinsky, I. and Teshima, M. and Tibaldo, L. and Tibolla, O. and Tovmassian, G. and Travnicek, P. and Trzeciak, M. and Vallania, P. and van Eldik, C. and Vercellone, S. and Vigorito, C. and Wagner, S.J. and Wakely, S.P. and Weinstein, A. and Wierzcholska, A. and Wilhelm, A. and Wojcik, P. and Yoshikoshi, T. (2015) 'The Cherenkov Telescope Array potential for the study of young supernova remnants.', Astroparticle physics., 62 . pp. 152-164.
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.
|Keywords:||Acceleration of particles, Gamma rays, General, ISM: Supernova remnants, Radiation mechanisms: Non-termal.|
|Full text:||(AM) Accepted Manuscript|
Available under License - Creative Commons Attribution Non-commercial No Derivatives.
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|Publisher Web site:||https://doi.org/10.1016/j.astropartphys.2014.08.005|
|Publisher statement:||© 2014 This manuscript version is made available under the CC-BY-NC-ND 4.0 license http://creativecommons.org/licenses/by-nc-nd/4.0/|
|Date accepted:||30 August 2014|
|Date deposited:||01 June 2018|
|Date of first online publication:||28 September 2014|
|Date first made open access:||No date available|
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