The Cherenkov Telescope Array potential for the study of young supernova remnants

Acharya, B. S.; Aramo, C.; Babić, Ana; Barrio, J. A.; Baushev, A. N.; Tjus, J. Becker; Berge, D.; Bohã̌cov́a, M.; Bonardi, A.; Brown, A. M.; Bugaev, V.; Bulik, T.; Burton, M. G.; Busetto, G.; Caraveo, P. A.; Carosi, R.; Carr, J.; Chadwick, P. M.; Chudoba, J.; Conforti, Vito; Connaughton, V.; Contreras, J. L.; Cotter, Garret; Dazzi, F.; Franco, Andrea; Calle, I. de la; Lopez, R. de los Reyes; Lotto, B. De; Palma, F. de; Girolamo, T. Di; Giulio, C. Di; Pierro, F. Di; Dournaux, Jean-Laurent; Dwarkadas, Vikram V.; Ebr, Jan; Egberts, K.; Fesquet, M.; Fleischhack, Henrike; Font, L.; Fontaine, G.; Förster, A.; Fuessling, Matthias; García, Beatriz; López, Rebeca; Garczarczyk, M.; Gargano, F.; Garrido, Daniel; Gaug, M.; Giglietto, N.; Giordano, F.; Giuliani, A.; Godinović, N.; González, M. M.; Grabarczyk, T.; Hassan, Tarek; Hörandel, J. R.; Hrabovský, M.; Hrupec, Dario; Humensky, T. B.; Huovelin, J.; Jamrozy, M.; Janeček, Petr; Kaaret, Philip; Katz, U.; Kaufmann, S.; Khélifi, B.; Kluźniak, W.; Kocot, Joanna; Komin, Nu.; Kubo, H.; Kushida, J.; Lamanna, G.; Lee, W.H.; Lenain, J.‐P.; Löhse, T.; Lombardi, S.; López-Coto, R.; López-Oramas, A.; Lucarelli, F.; Maccarone, M. C.; Maier, G.; Majumdar, P.; Malaguti, G.; Mandat, D.; Mazziotta, M. N.; Meagher, K.; Mirabal, N.; Morselli, A.; Moulin, Emmanuel; Niemiec, J.; Nievas, Mireia; Nishijima, K.; Nosek, D.; Nunio, F.; Ohishi, M.; Ohm, S.; Ong, R. A.; Orito, R.; Otte, N.; Palatka, M.; Pareschi, G.; Pech, M.; Peršić, M.; Pohl, M.; Prouza, M.; Quirrenbach, A.; Rainò, S.; Fernandez, G. Rodriguez; Romano, P.; Rovero, A. C.; Rudak, B.; Schovánek, Petr; Shayduk, M.; Siejkowski, Hubert; Sillanpää, A.; Stefanik, Stanislav; Stolarczyk, Th.; Szanecki, Michał; Szepieniec, Tomasz; Tejedor, Luis; Telezhinsky, I.; Teshima, M.; Tibaldo, L.; Tibolla, O.; Tovmassian, G.; Trávničék, P.; Trzeciak, M.; Vallania, P.; Eldik, C. van; Vercellone, S.; Vigorito, C.; Wagner, S. J.; Wakely, S. P.; Weinstein, A. J.R.; Wierzcholska, A.; Wilhelm, A.; Wojcik, Pamela Robertson; Yoshikoshi, T.

doi:10.1016/j.astropartphys.2014.08.005

Cited by 7 publications

(3 citation statements)

References 46 publications

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“…The investigation of complex morphological models for SNRs, as for example discussed in (Meyer et al, 2021), is beyond the scope of this work. The potential of CTA to detect and spatially resolve young SNRs is discussed in detail in Acero et al (2013); Acharya et al (2015); Mitchell et al (2021). Due to its dependence on a simplified model for the distribution, evolution and 𝛾-ray emission of SNRs in the Galaxy, the result for the number of Galactic SNRs which can be detected by CTA is considered only as a benchmark result which is valid only within the assumptions of the model.…”

Section: Search For Snr Pevatrons With Ctamentioning

confidence: 99%

Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants

Angüner¹,

Spengler²,

Costantini³

et al. 2023

Astroparticle Physics

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Section: Search For Snr Pevatrons With Ctamentioning

confidence: 99%

Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants

Angüner¹,

Spengler²,

Costantini³

et al. 2023

Astroparticle Physics

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“…Most of the core-collapse SNRs require a thorough numerical modeling, while type-Ia SNRs can be well described analytically. Besides, it was shown (Acharya et al 2015) that type-Ia SNRs should be easiest to observe with the future CTA facility owing to a continuous increase of γ-ray flux and size. For many core-collapse SNRs detectability and resolvability is a strong function of the age.…”

Section: Evolution Of Supernova Remnantmentioning

confidence: 99%

Transport of magnetic turbulence in supernova remnants

Brose

Telezhinsky

Pohl

2016

A&A

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Context. Supernova remnants are known as sources of galactic cosmic rays for their non-thermal emission of radio waves, X-rays, and gamma-rays. However, the observed soft broken power-law spectra are hard to reproduce within standard acceleration theory based on the assumption of Bohm diffusion and steady-state calculations.Aims. We point out that a time-dependent treatment of the acceleration process together with a self-consistent treatment of the scattering turbulence amplification is necessary. Methods. We numerically solve the coupled system of transport equations for cosmic rays and isotropic Alfvénic turbulence. The equations are coupled through the growth rate of turbulence determined by the cosmic-ray gradient and the spatial diffusion coefficient of cosmic rays determined by the energy density of the turbulence. The system is solved on a co-moving expanding grid extending upstream for dozens of shock radii, allowing for the self-consistent study of cosmic-ray diffusion in the vicinity of their acceleration site. The transport equation for cosmic rays is solved in a test-particle approach.Results. We demonstrate that the system is typically not in a steady state. In fact, even after several thousand years of evolution, no equilibrium situation is reached. The resulting time-dependent particle spectra strongly differ from those derived assuming a steady state and Bohm diffusion. Our results indicate that proper accounting for the evolution of the scattering turbulence and hence the particle diffusion coefficient is crucial for the formation of the observed soft spectra. In any case, the need to continuously develop magnetic turbulence upstream of the shock introduces non-linearity in addition to that imposed by cosmic-ray feedback.

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“…Radio surveys which are commonly used to identify SNRs are biased against small angular diameter SNRs, as would be the case for a young remnant on the other side of the Galaxy. Future surveys with CTA could reach sufficient sensitivity to take a census of the young Galactic SNRs [39].…”

Section: Other Young Galactic Supernova Remnantsmentioning

confidence: 99%

Observations of supernova remnants and pulsar wind nebulae at gamma-ray energies

Hewitt

Lemoine‐Goumard

2015

Comptes Rendus. Physique

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International audienceIn the past few years, gamma-ray astronomy has entered a golden age thanks to two major breakthroughs: Cherenkov telescopes on the ground and the Large Area Telescope (LAT) onboard the Fermi satellite. The sample of supernova remnants (SNRs) detected at gamma-ray energies is now much larger: it goes from evolved supernova remnants interacting with molecular clouds up to young shell-type supernova remnants and historical supernova remnants. Studies of SNRs are of great interest, as these analyses are directly linked to the long standing issue of the origin of the Galactic cosmic rays. In this context, pulsar wind nebulae (PWNe) need also to be considered since they evolve in conjunction with SNRs. As a result, they frequently complicate interpretation of the gamma-ray emission seen from SNRs and they could also contribute directly to the local cosmic ray spectrum, particularly the leptonic component. This paper reviews the current results and thinking on SNRs and PWNe and their connection to cosmic ray production

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The Cherenkov Telescope Array potential for the study of young supernova remnants

Cited by 7 publications

References 46 publications

Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants

Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants

Transport of magnetic turbulence in supernova remnants

Observations of supernova remnants and pulsar wind nebulae at gamma-ray energies

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