Postshock turbulence and diffusive shock acceleration in young supernova remnants

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Table 2:

Inferred values of the downstream magnetic field amplitude and synchrotron photon cut-off energy in the case of an *advection-dominated* rim where Bohm diffusion regime prevails ( $\beta =1$ and $q(\beta =1)=\sigma$ ).
Supernova remnant	$B_{\rm d} \ (\mu G)$	$\displaystyle \frac{E_{\rm\gamma-cut}}{E_{\rm\gamma-cut,obs}}$	$B_{\rm d-FII}\ (mG)$
Cas A	558	0.2	2.7
Kepler	433	0.3	2.3
Tycho	586	0.7	1.5
SN 1006	170	0.07	0.56
G347.3-0.5	131	0.05	2.1

Notes. The magnetic field values were calculated by assuming $r_{\rm tot}=r_{\rm sub} = 4$ .

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