We compare the physical parameters and the relative abundances calculated throughout supernova ( SN ) and \gamma -ray burst ( GRB ) host galaxies by the detailed modelling of the spectra .
The coupled effect of shocks and radiation from the starburst within the host galaxy is considered .
We have found that 1 ) shock velocities are lower in long period GRB ( LGRB ) than in SN host galaxies .
2 ) O/H relative abundances in SN hosts are scattered within a range 8.0 < 12+log ( O/H ) < 8.85 but they are close to solar in LGRB hosts .
LGRB galaxies hosting Wolf-Rayet ( WR ) stars have He/H=0.13 in a few objects .
3 ) The starburst temperatures within a few SN hosts are relatively high ( T _ { * } > 10 ^ { 5 } K ) . T _ { * } in LGRB hosts are \sim 3-8 10 ^ { 4 } K. 4 ) The H { \alpha } absolute flux calculated from the emitting clouds of a few SN hosts at 0.1 < z < 0.3 is sensibly higher than in the other galaxies .
H { \alpha } increases sharply with the ionization parameter U .
The present analysis suggests that the SN-host symbiosis is stronger than for GRB in terms of activity .
The physical and chemical conditions in the GRB host galaxies are similar to those in SB galaxies within a large z range .