Effective Helium Burning Rates and the Production of the Neutrino Nuclei

Abstract

Effective values for the key helium burning reaction rates, triple-alpha and 12C(alpha,gamma)16O, are obtained by adjusting their strengths so as to obtain the best match with the solar abundance pattern of isotopes uniquely or predominately made in core collapse supernovae. These effective rates are then used to determine the production of the neutrino isotopes. The use of effective rates considerably reduces the uncertainties in the production factors arising from uncertainties in the helium burning rates, and improves our ability to use the production of 11B to constrain the neutrino emission from supernovae.

Accepted for publication in Physical Review Letters

References in corpus (5)

• Nucleosynthesis and Remnants in Massive Stars of Solar Metallicity
• The Compactness of Presupernova Stellar Cores
• On the Sensitivity of Massive Star Nucleosynthesis and Evolution to Solar Abundances and to Uncertainties in Helium Burning Reaction Rates
• Dependence of S-Process Nucleosynthesis in Massive Stars on Triple-Alpha and 12C(a,g)16O Reaction Rate Uncertainties
• 11B and Constraints on Neutrino Oscillations and Spectra from Neutrino Nucleosynthesis

Cited by in corpus (11)

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• The $\nu$ process in the light of an improved understanding of supernova neutrino spectra
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• Resolving The Peak Of The Black Hole Mass Spectrum
• It's written in the massive stars: The role of stellar physics in the formation of black holes
• Supernova Neutrino Process of Li and B Revisited
• Astrophysical S factor of {${}^{12}$C($\alpha ,\gamma$)${}^{16}$O} Calculated with the Reduced R-matrix Theory
• Reducing Uncertainties in the Production of the Gamma Emitting Nuclei 26Al, 44Ti, and 60Fe in Core Collapse Supernovae by Using Effective Helium Burning Rates
• Effects of Triple-$\alpha$ and ${}^{12}\mathrm{C}(\alpha ,\gamma {)}^{16}\mathrm{O}$ Reaction Rates on the Supernova Nucleosynthesis in a Massive Star of 25 $M_{\odot }$
• Measurement of the branching ratio for beta-delayed alpha decay of 16N
• Reaction rate weighted multilayer nuclear reaction network