Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21713002c&link_type=abstract
American Astronomical Society, AAS Meeting #217, #130.02; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
Observational evidence increasingly supports the scenario where cosmic rays are accelerated at supernova remnant (SNR) shocks. Both thermal and non-thermal emission from these objects, in a wide range of wavelengths, indicate the presence of extremely energetic particles in SNRs, and the development of analytical and semi-analytical models of SNR evolution where diffusive shock acceleration (DSA) is efficient allow for constraining the nature of cosmic ray production.
The research presented in this talk focuses on the impact of DSA on the evolution and observational properties of SNRs, and it is divided in three main parts. Firstly, an X-ray study of the morphology and spectral properties of SNR G296.1-0.5 is performed, using the XMM-Newtonn X-ray Observatory. Modeling of the observational characteristics of this SNR suggest the remnant is in the adiabatic expansion phase, and is possibly the result of the core collapse of a massive progenitor. The detection of a bursting compact source in the direction of the remnant, and its nature and possible association with the SNR, is also discussed. Secondly, a semi-analytical model is presented, which considers the modifications to the evolution and emission characteristics of SNRs in the Sedov-Taylor phase, imposed by DSA. This study shows how efficient cosmic ray acceleration impacts the analysis of SNRs in this evolution phase, and how the results diverge from the standard model when the acceleration process is efficient. Finally, the gamma-ray observations, with the Fermi LAT, of MeV-GeV emission coincident with four SNRs are analyzed. These SNRs show evidence of interaction with dense molecular clouds, from OH maser studies, and the gamma-ray emission in their directions is explained in this study as the result of pion-decay emission from the dense molecular material interacting with cosmic rays accelerated at the shocks of these remnants.
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