We perform hydrodynamical and nucleosynthesis calculations of core-collapse supernovae ( SNe ) and hypernovae ( HNe ) of Population ( Pop ) III stars .
We provide new yields for the main-sequence mass of M _ { MS } = 13 - 50 M _ { \odot } and the explosion energy of E = 1 - 40 \times 10 ^ { 51 } ergs to apply for chemical evolution studies .
Our HN yields based on the mixing-fallback model of explosions reproduce the observed abundance patterns of extremely metal-poor ( EMP ) stars ( -4 < { [ Fe / H ] } < -3 ) , while those of very metal-poor ( VMP ) stars ( -3 < { [ Fe / H ] } < -2 ) are reproduced by the normal SN yields integrated over the Salpeter initial mass function .
Moreover , the observed trends of abundance ratios [ X/Fe ] against [ Fe/H ] with small dispersions for the EMP stars can be reproduced as a sequence resulting from the various combination of M _ { MS } and E .
This is because we adopt the empirical relation that a larger amount of Fe is ejected by more massive HNe .
Our results imply that the observed trends with small dispersions do not necessarily mean the rapid homogeneous mixing in the early galactic halo at [ Fe/H ] < -3 , but can be reproduced by the “ inhomogeneous ” chemical evolution model .
In addition , we examine how the modifications of the distributions of the electron mole fraction Y _ { e } and the density in the presupernova models improve the agreement with observations .
In this connection , we discuss possible contributions of nucleosynthesis in the neutrino-driven wind and the accretion disk .