Many works have found unusual characteristics of elemental abundances in nearby dwarf galaxies .
This implies that there is a key factor of galactic evolution that is different from that of the Milky Way ( MW ) .
The chemical abundances of the stars in the Fornax dwarf spheroidal galaxy ( Fornax dSph ) provide excellent information for setting constraints on the models of the galactic chemical evolution .
In this work , adopting the five-component approach , we fit the abundances of the Fornax dSph stars , including \alpha elements , iron group elements and neutron-capture elements .
For most sample stars , the relative contributions from the various processes to the elemental abundances are not usually in the MW proportions .
We find that the contributions from massive stars to the primary \alpha elements and iron group elements increase monotonously with increasing [ Fe/H ] .
This means that the effect of the galactic wind is not strong enough to halt star formation and the contributions from massive stars to \alpha elements did not halted for [ Fe/H ] \lesssim -0.5 .
The average contributed ratios of various processes between the dSph stars and the MW stars monotonously decrease with increasing progenitor mass .
This is important evidence of a bottom-heavy initial mass function ( IMF ) for the Fonax dSph , compared to the MW .
Considering a bottom-heavy IMF for the dSph , the observed relations of [ \alpha /Fe ] versus [ Fe/H ] , [ iron group/Fe ] versus [ Fe/H ] and [ neutron-capture/Fe ] versus [ Fe/H ] for the dSph stars can be explained .