MAGNETOROTATIONALLY DRIVEN SUPERNOVAE AS THE ORIGIN OF EARLY GALAXY r -PROCESS ELEMENTS?

We examine magnetorotationally driven supernovae as sources of r-process elements in the early Galaxy. On the basis of thermodynamic histories of tracer particles from a three-dimensional magnetohydrodynamical core-collapse supernova model with approximated neutrino transport, we perform nucleosynth...

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Bibliographic Details
Published in:Astrophysical journal. Letters 2012-05, Vol.750 (1), p.1-5
Main Authors: WINTELER, C, KAPPELI, R, Perego, A, Arcones, A, Vasset, N, Nishimura, N, Liebendorfer, M, Thielemann, F-K
Format: Article
Language:English
Subjects:
Approximation
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
COSMIC NEUTRINOS
Ejecta
GALACTIC EVOLUTION
GALAXIES
GRAVITATIONAL COLLAPSE
High Energy Astrophysical Phenomena
Jets
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
Neutrinos
NEUTRON STARS
NUCLEOSYNTHESIS
Progenitors (astrophysics)
R PROCESS
ROTATION
Sciences of the Universe
SUPERNOVAE
Three dimensional
THREE-DIMENSIONAL CALCULATIONS
Transport
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Summary:We examine magnetorotationally driven supernovae as sources of r-process elements in the early Galaxy. On the basis of thermodynamic histories of tracer particles from a three-dimensional magnetohydrodynamical core-collapse supernova model with approximated neutrino transport, we perform nucleosynthesis calculations with and without considering the effects of neutrino absorption reactions on the electron fraction (Y sub(e)) during post-processing. We find that the peak distribution of Y sub(e) in the ejecta is shifted from ~0.15 to ~0.17 and broadened toward higher Y sub(e) due to neutrino absorption. Nevertheless, in both cases, the second and third peaks of the solar r-process element distribution can be reproduced well. The rare progenitor configuration that was used here, characterized by a high rotation rate and a large magnetic field necessary for the formation of bipolar jets, could naturally provide a site for the strong r-process in agreement with observations of the early Galactic chemical evolution.
ISSN:2041-8205
2041-8213
DOI:10.1088/2041-8205/750/1/L22