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The recently discovered phosphorus-rich stars pose a challenge to stellarevolution and nucleosynthesis theory, as none of the existing models canexplain their extremely peculiar chemical abundances pattern. Apart from thelarge phosphorus enhancement, such stars also show enhancement in other light(O, Mg, Si, Al) and heavy (e.g., Ce) elements. We have obtained high-resolutionoptical spectra of two optically bright phosphorus-rich stars (including a newP-rich star), for which we have deter-mined a larger number of elementalabundances (from C to Pb). We confirm the unusual light-element abundancepattern with very large enhancements of Mg, Si, Al, and P, and possibly some Cuenhancement, but the spectra of the new P-rich star is the only one to revealsome C(+N) enhancement.When compared to other appropriate metal-poor andneutron-capture enhanced stars, the two P-rich stars show heavy-elementoverabundances similar to low neutron density s-process nucleosynthesis,withhigh first- (Sr, Y, Zr) and second-peak (Ba, La, Ce, Nd) element enhancements(even some Pb enhancement in one star) and a negative [Rb/Sr] ratio. However,this s-process is distinct from the one occurring in asymptotic giant branch(AGB) stars. The notable distinctions encompass larger[Ba/La] and lower Eu andPb than their AGB counterparts. Our observations should guide stellarnucleosynthesis theoreticians and observers to identify the P-rich starprogenitor, which represents anew site for s-process nucleosynthesis, withimportant implications for the chemical evolution of our Galaxy.

Heavy element abundances in P-rich stars: A new site for the s-process?