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We propose magnetic proto-neutron star (PNS) winds driven by \Alfven waves aswell as the neutrino heating as an appropriate site for the r-processnucleosynthesis. \Alfven waves excited by surface motions of a PNS propagateoutwardly, and they heat and accelerate the wind by dissipation. Compared withthe wind purely driven by the neutrino heating, larger entropy per baryon andshorter dynamical time scale are achieved, which favors the r-process. We studyreasonable cases that a wave amplitude is 10% of \Alfven speed at the surfaceto find that a PNS with surface field strength, $\gtrsim 5\times 10^{14}$G,gives suitable wind properties for the r-process, provided that dissipationlength of the wave is at most $\sim$ 10 times of the PNS radius. We alsocompare properties of transcritical and subcritical winds in light of ther-process. We finally discuss possibilities of detections of $\gamma$-rays fromradioactive nuclei and absorption lines due to Ba in supernova remnants whichpossess magnetars.Comment: 14 pages, including 4 figures, ApJ, in pres

Alfven Wave–driven Proto–Neutron Star Winds andr‐Process Nucleosynthesis