It is shown that the nonlinear kinetic model of cosmic ray ( CR ) acceleration in supernova remnants ( SNRs ) fits the shell-type nonthermal X-ray morphology , obtained in Chandra observations , in a satisfactory way .
The set of empirical parameters is the same which reproduces the dynamical properties of the SNR and the spectral characteristics of the emission produced by CRs .
The extremely small spatial scales of the observed X-ray distribution are due to the large effective magnetic field B _ { \mathrm { d } } \sim 100 \mu G in the interior , which is also required to give a good fit for the spatially integrated radio and X-ray synchrotron spectra .
The only reasonably thinkable condition for the production of such a large effective field strength is an efficiently accelerated nuclear CR component .
Therefore the Chandra data confirm the inference that SN 1006 indeed accelerates nuclear CRs with the high efficiency required for SNRs to be considered as the main Galactic CR sources .