Abstract
We propose magnetic proto-neutron star (PNS) winds driven by Alfvén waves, as well as the neutrino heating, as an appropriate site for r-process nucleosynthesis. Alfvén waves excited by surface motions of a PNS propagate outwardly, and they heat and accelerate the wind by dissipation. Compared with the wind purely driven by neutrino heating, a larger entropy per baryon and shorter dynamical timescale are achieved, which favors the r-process. We study reasonable cases in which the wave amplitude is 10% of the Alfvén speed at the surface to find that a PNS with surface field strength ≳5 × 1014 G gives suitable wind properties for the r-process, provided that the dissipation length of the wave is at most ~10 times the PNS radius. We also compare properties of transcritical and subcritical winds in light of the r-process. We finally discuss possibilities of detections of γ-rays from radioactive nuclei and absorption lines due to Ba in supernova remnants that possess magnetars.
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