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We have performed large-scale nucleosynthesis calculations within thehigh-entropy-wind (HEW) scenario of type II supernovae. The primary aim was toconstrain the conditions for the production of the classical "p-only" isotopesof the light trans-Fe elements. We find, however, that for electron fractionsin the range 0.458 $\le$ Y$_e$ $\le$ 0.478, sizeable abundances of p-, s- andr-process nuclei between $^{64}$Zn and $^{98}$Ru are coproduced in the HEW atlow entropies (S $\le$ 100) by a primary charged-particle process after an$\alpha$-rich freezeout. With the above Y$_e$ -- S correlation, most of thepredicted isotopic abundance ratios within a given element (e.g.$^{64}$Zn(p)/$^{70}$Zn(r) or $^{92}$Mo(p)/$^{94}$Mo(p)), as well as ofneighboring elements (e.g. $^{70}$Ge(s+p)/$^{74}$Se(p) or$^{74}$Se(p)/$^{78}$Kr(p)) agree with the observed Solar-System ratios. Takingthe Mo isotopic chain as a particularly challenging example, we show that ourHEW model can account for the production of all 7 stable isotopes, from"p-only" $^{92}$Mo, via "s-only" $^{96}$Mo up to "r-only" $^{100}$Mo.Furthermore, our model is able to reproduce the isotopic composition of Mo inpresolar SiC X-grains.}

Co-production of light p-, s- and r-process isotopes in the high-entropy wind of type II supernovae