Magnetic Field in Supernova Remnant SN 1987A

A nonlinear kinetic theory of cosmic-ray (CR) acceleration in supernova remnants is employed to investigate the properties of the remnant SN 1987A. It is shown that a large downstream magnetic field B sub(d) -10 mG is required to fit the existing observational data. Such a strong field, together with the strong shock modification due to CR back-reaction, provides the steep and concave radioemission spectrum and considerable synchrotron cooling of high-energy electrons that diminish their X-ray synchrotron flux below the observed Chandra flux, which has to be considered as an upper limit for nonthermal X-ray emission. The expected g-ray energy flux at TeV energies at the current epoch is 2 x 10 super(-13) ergs (cm super(2) s) super(-1).