Abstract
Neutrino-driven winds are thought to accompany the Kelvin-Helmholtz cooling phase of nascent protoneutron stars in the first seconds after a core-collapse supernova. These outflows are a likely candidate as the astrophysical site for rapid neutron-capture nucleosynthesis (the r-process). In this chapter we review the physics of protoneutron star winds and assess their potential as a site for the production of the heavy r-process nuclides. We show that spherical transonic protoneutron star winds do not produce robust r-process nucleosynthesis for ‘canonical’ neutron stars with gravitational masses of 1.4 M⊙ and coordinate radii of 10 km.
We further speculate on and review some aspects of neutrino-driven winds from protoneutron stars with strong magnetic fields.
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Thompson, T.A. (2004). Protoneutron Star Winds. In: Fryer, C.L. (eds) Stellar Collapse. Astrophysics and Space Science Library, vol 302. Springer, Dordrecht. https://doi.org/10.1007/978-0-306-48599-2_6
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