This paper investigates the origin of the observed large variety in dust-to-gas ratio , \cal { D } , among blue compact dwarf galaxies ( BCDs ) .
By applying our chemical evolution model , we find that the dust destruction can largely suppress the dust-to-gas ratio when the metallicity of a BCD reaches 12 + \log { ( O / H ) } \sim 8 , i.e. , a typical metallicity level of BCDs .
We also show that dust-to-gas ratio is largely varied owing to the change of dust destruction efficiency that has two effects : ( i ) a significant contribution of Type Ia supernovae to total supernova rate ; ( ii ) variation of gas mass contained in a star-forming region .
While mass loss from BCDs was previously thought to be the major cause for the variance of \cal { D } , we suggest that the other two effects are also important .
We finally discuss the intermittent star formation history , which naturally explains the large dispersion of dust-to-gas ratio among BCDs .