The nonlinear kinetic model of cosmic ray ( CR ) acceleration in supernova remnants ( SNRs ) is used to describe the properties of the remnant of SN 1006 .
It is shown , that the theory fits the existing data in a satisfactory way within a set of parameters which is consistent with the idea that SN 1006 is a typical source of Galactic CR nucleons , although not necessarily of CR electrons .
The adjusted parameters are those that are not very well determined by present theory or not directly amenable to astronomical observations .
The calculated expansion law and the radio- , X-ray and \gamma -ray emissions produced by the accelerated CRs in SN 1006 agree quite well with the observations .
A rather large interior magnetic field B _ { \mathrm { d } } \approx 100 \mu G is required to give a good fit for the radio and X-ray synchrotron emission .
In the predicted TeV \gamma -ray flux from SN 1006 , the \pi ^ { 0 } -decay \gamma -rays , generated by the nuclear CR component , dominate over the inverse Compton ( IC ) \gamma -rays , generated by the CR electrons in the cosmic microwave background .
The predicted source morphology in high energy \gamma -rays roughly corresponds to that of the synchrotron emission .
The predicted integral \gamma -ray flux F _ { \gamma } \propto \epsilon _ { \gamma } ^ { -1 } extends up to energies \sim 100 TeV if CR diffusion is as strong as the Bohm limit .
Only if the interior magnetic field is much lower in the SNR , B _ { \mathrm { d } } \approx 10 \mu G , then the observed \gamma -ray emission can be due to the accelerated electron component alone .
In this case , not plausible physically in our view , the lowest permissible value of the electron to proton ratio is rather high , and the maximum individual energy and total energy content of accelerated nucleons so small , that SN 1006 can not be considered as a typical source of the nuclear Galactic CRs .