paper

Rapid-Process Nucleosynthesis in Neutrino-Magneto-Centrifugally Driven Winds

arXiv:astro-ph/0101347 · doi:10.1093/pasj/53.3.547

Abstract

We have studied whether the rotation and magnetic fields in neutrino-driven winds can be key processes for the rapid-process (r-process) nucleosynthesis. We have examined the features of a steady and subsonic wind solutions which extend the model of Weber and Davis (1967), which is a representative solar wind model. As a result, we found that the entropy per baryon becomes lower and the dynamical timescale becomes longer as the angular velocity becomes higher. These results are inappropriate for the production of the r-process nuclei. As for the effects of magnetic fields, we found that a solution as a steady wind from the surface of the proto-neutron star can not be obtained when the strength of the magnetic field becomes G. Since the magnetic field in normal pulsars is of order G, a steady wind solution might not be realized there, which means that the models in this study may not be adopted for normal proto-neutron stars. In this situation, we have little choice but to conclude that it is difficult to realize a successful r-process nucleosynthesis in the wind models in this framework.

20 pages and 4 postscript figures. submitted to Publications of the Astronomical Society of Japan

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