  Current r-process models under-produce A<130 nuclei. P-process models either
underproduce A<100 and 150<A<165 p-nuclei, or have other limitations. We argue
that the puzzles in these two mechanisms can be solved by heavy-ion spallation.
Spallation happens in the explosive phase transition from a neutron star to a
quark star - the quark-nova. The quark-nova triggers the r-process which
creates abundant A>130 nuclei, and spallation fragments these isotopes into
A<130 nuclei and all 35 p-nuclei. Our model is universal in relation to a
star's age, metallicity, and chemistry.
