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      Detection of the Characteristic Pion-Decay Signature in Supernova Remnants

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      American Association for the Advancement of Science (AAAS)

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          Nonlinear theory of diffusive acceleration of particles by shock waves

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            Extremely fast acceleration of cosmic rays in a supernova remnant

            Galactic cosmic rays (CRs) are widely believed to be accelerated by shock waves associated with the expansion of supernova ejecta into the interstellar medium. A key issue in this long-standing conjecture is a theoretical prediction that the interstellar magnetic field can be substantially amplified at the shock of a young supernova remnant (SNR) through magnetohydrodynamic waves generated by cosmic rays. Here we report a discovery of the brightening and decay of X-ray hot spots in the shell of the SNR RX J1713.7-3946 on a one-year timescale. This rapid variability shows that the X-rays are produced by ultrarelativistic electrons through a synchrotron process and that electron acceleration does indeed take place in a strongly magnetized environment, indicating amplification of the magnetic field by a factor of more than 100. The X-ray variability also implies that we have witnessed the ongoing shock-acceleration of electrons in real time. Independently, broadband X-ray spectrometric measurements of RX J1713.7-3946 indicate that electron acceleration proceeds in the most effective ('Bohm-diffusion') regime. Taken together, these two results provide a strong argument for acceleration of protons and nuclei to energies of 1 PeV (10(15) eV) and beyond in young supernova remnants.
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              Cosmic‐Ray Acceleration at the Forward Shock in Tycho’s Supernova Remnant: Evidence fromChandraX‐Ray Observations

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                Author and article information

                Journal
                Science
                Science
                American Association for the Advancement of Science (AAAS)
                0036-8075
                1095-9203
                February 14 2013
                February 15 2013
                February 14 2013
                February 15 2013
                : 339
                : 6121
                : 807-811
                Article
                10.1126/science.1231160
                23413352
                d1772f4e-94ba-439d-bd7e-2ff19b4c020c
                © 2013
                History

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