The Nucleosynthetic Yields of Core-Collapse Supernovae, prospects for the Next Generation of Gamma-Ray Astronomy. (arXiv:1912.10542v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Andrews_S/0/1/0/all/0/1">Sydney Andrews</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fryer_C/0/1/0/all/0/1">Chris L. Fryer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_S/0/1/0/all/0/1">Samuel W. Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Even_W/0/1/0/all/0/1">Wesley P. Even</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pignatari_M/0/1/0/all/0/1">Marco Pignatari</a>
Though the neutrino-driven convection model for the core-collapse explosion
mechanism has received strong support in recent years, there are still many
uncertainties in the explosion parameters — such as explosion energy, remnant
mass, and end-of-life stellar abundances as initial conditions. Using a broad
set of spherically symmetric core-collapse simulations we examine the effects
of these key parameters on explosive nucleosynthesis and final explosion
yields. Post-bounce temperature and density evolution of ZAMS 15, 20, and 25
solar mass progenitors are post-processed through the Nucleosynthesis Grid
(NuGrid) nuclear network to obtain detailed explosive yields. In particular,
this study focuses on radio-isotopes that are of particular interest to the
next generation of gamma-ray astronomical observations; 43K, 47Ca, 44Sc, 47Sc,
48V, 48Cr, 51Cr, 52Mn, 59Fe, 56Co, 57Co, 57Ni. These nuclides may be key in
advancing our understanding of the inner workings of core-collapse supernovae
by probing the parameters of the explosion engine. We find that the isotopes
that are strong indicators of explosion energy are 43K, 47Ca, 44Sc, 47Sc, and
59Fe, those that are dependent on the progenitor structure are 48V, 51Cr, and
57Co, and those that probe neither are 48Cr, 52Mn, 57Ni, and 56Co. We discuss
prospects of observing these radionuclides in supernova remnants.
Though the neutrino-driven convection model for the core-collapse explosion
mechanism has received strong support in recent years, there are still many
uncertainties in the explosion parameters — such as explosion energy, remnant
mass, and end-of-life stellar abundances as initial conditions. Using a broad
set of spherically symmetric core-collapse simulations we examine the effects
of these key parameters on explosive nucleosynthesis and final explosion
yields. Post-bounce temperature and density evolution of ZAMS 15, 20, and 25
solar mass progenitors are post-processed through the Nucleosynthesis Grid
(NuGrid) nuclear network to obtain detailed explosive yields. In particular,
this study focuses on radio-isotopes that are of particular interest to the
next generation of gamma-ray astronomical observations; 43K, 47Ca, 44Sc, 47Sc,
48V, 48Cr, 51Cr, 52Mn, 59Fe, 56Co, 57Co, 57Ni. These nuclides may be key in
advancing our understanding of the inner workings of core-collapse supernovae
by probing the parameters of the explosion engine. We find that the isotopes
that are strong indicators of explosion energy are 43K, 47Ca, 44Sc, 47Sc, and
59Fe, those that are dependent on the progenitor structure are 48V, 51Cr, and
57Co, and those that probe neither are 48Cr, 52Mn, 57Ni, and 56Co. We discuss
prospects of observing these radionuclides in supernova remnants.
http://arxiv.org/icons/sfx.gif
