Effective helium burning rates and the production of the neutrino nuclei.
Effective values for the key helium burning reaction rates, triple-α and (12)C(α, γ)(16)O, 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 B11 to constrain the neutrino emission from supernovae.
National Superconducting Cyclotron Laboratory, Michigan State University, 640 South Shaw Lane, East Lansing, Michigan 48824-1321, USA and Joint Institute for Nuclear Astrophysics, University of Notre Dame, Notre Dame IN 46545, USA.
Sam M
SM
Austin
Joint Institute for Nuclear Astrophysics, University of Notre Dame, Notre Dame IN 46545, USA and Minnesota Institute for Astronomy, School of Physics and Astronomy, The University of Minnesota, Twin Cities, Minneapolis, Minnesota 55455-0149, USA.
Christopher
C
West
Joint Institute for Nuclear Astrophysics, University of Notre Dame, Notre Dame IN 46545, USA and Minnesota Institute for Astronomy, School of Physics and Astronomy, The University of Minnesota, Twin Cities, Minneapolis, Minnesota 55455-0149, USA and Monash Centre for Astrophysics, School of Mathematical Sciences, Monash University, Victoria 3800, Australia.
Alexander
A
Heger