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Protoneutron Star Winds

  • Todd A. Thompson
Part of the Astrophysics and Space Science Library book series (ASSL, volume 302)

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.

Keywords

nuclear reactions nucleosynthesis abundances—stars: magnetic fields—stars: winds outflows—stars: neutron—supernovae: general 

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Copyright information

© Springer Science+Business Media Dordrecht 2004

Authors and Affiliations

  • Todd A. Thompson
    • 1
  1. 1.Astronomy Department and Theoretical Astrophysics CenterThe University of CaliforniaBerkeleyUSA

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