We present BeppoSAX X-ray spectra of the remnant of the supernova of AD 1006 , which cover a broad spectral range of 0.1-10 keV .
In our analysis we concentrate on the thermal emission from the central region of the remnant .
For this purpose we fitted the spectra of the whole remnant using a new version of the spectral program SPEX , which takes into account the interdependence of spectra of different regions as the result of the point spread function of the instruments .
This is in particular important for separating the synchrotron emission , coming from the bright rims of the remnant , from the thermal emission from the central regions .

The thermal emission appears best fitted with a combination of two spectral components with electron temperatures of \sim 0.7 keV and \buildrel > \over { \sim } 3 keV .
The plasma in SN 1006 appears to be very far out of ionization equilibrium ( n _ { e } t \sim 2 10 ^ { 15 } m ^ { -3 } s ) , which means that the L-shell emission of magnesium , silicon and sulphur contribute significantly to the flux below 0.5 keV .
We also note the presence of Fe K line emission at 6.3 \pm 0.2 keV , in agreement with an origin from inner shell ionizations and excitations .
We confirm that the abundances in SN 1006 are clearly non-solar .
In particular silicon is very abundant .
We did not find substantial variations in plasma properties over the face of the remnant , although the hotter component seems more dominant in the Northern half of the remnant .