TRENDS IN {sup 44}Ti AND {sup 56}Ni FROM CORE-COLLAPSE SUPERNOVAE

Journal Article · Mon Nov 15 04:00:00 EST 2010 · Astrophysical Journal, Supplement Series

DOI:https://doi.org/10.1088/0067-0049/191/1/66· OSTI ID:21471247

Magkotsios, Georgios; Wiescher, Michael ^[1]; Timmes, F X; Young, Patrick A ^[2]; Hungerford, Aimee L; Fryer, Christopher L ^[3]

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1. Department of Physics, University of Notre Dame, Notre Dame, IN 46556 (United States)
2. School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287 (United States)
3. Los Alamos National Laboratory, Los Alamos, NM 87545 (United States)

We compare the yields of {sup 44}Ti and {sup 56}Ni produced from post-processing the thermodynamic trajectories from three different core-collapse models-a Cassiopeia A progenitor, a double shock hypernova progenitor, and a rotating two-dimensional explosion-with the yields from exponential and power-law trajectories. The peak temperatures and densities achieved in these core-collapse models span several of the distinct nucleosynthesis regions we identify, resulting in different trends in the {sup 44}Ti and {sup 56}Ni yields for different mass elements. The {sup 44}Ti and {sup 56}Ni mass fraction profiles from the exponential and power-law profiles generally explain the tendencies of the post-processed yields, depending on which regions are traversed by the model. We find that integrated yields of {sup 44}Ti and {sup 56}Ni from the exponential and power-law trajectories are generally within a factor two or less of the post-process yields. We also analyze the influence of specific nuclear reactions on the {sup 44}Ti and {sup 56}Ni abundance evolution. Reactions that affect all yields globally are the 3{alpha}, p(e{sup -}, {nu}{sub e})n and n(e{sup +},{nu}-bar{sub e})p. The rest of the reactions are ranked according to their degree of impact on the synthesis of {sup 44}Ti. The primary ones include {sup 44}Ti({alpha}, p){sup 47}V, {sup 40}Ca({alpha}, {gamma}){sup 44}Ti, {sup 45}V(p, {gamma}){sup 46}Cr, {sup 40}Ca({alpha}, p){sup 43}Sc, {sup 17}F({alpha}, p){sup 20}Ne, {sup 21}Na({alpha}, p){sup 24}Mg, {sup 41}Sc(p, {gamma}){sup 42}Ti, {sup 43}Sc(p, {gamma}){sup 44}Ti, {sup 44}Ti(p, {gamma}){sup 45}V, and {sup 57}Ni(p, {gamma}){sup 58}Cu, along with numerous weak reactions. Our analysis suggests that not all {sup 44}Ti need to be produced in an {alpha}-rich freeze-out in core-collapse events, and that reaction rate equilibria in combination with timescale effects for the expansion profile may account for the paucity of {sup 44}Ti observed in supernova remnants.

• OSTI ID: 21471247
• Journal Information: Astrophysical Journal, Supplement Series, Journal Name: Astrophysical Journal, Supplement Series Journal Issue: 1 Vol. 191; ISSN 0067-0049; ISSN APJSA2
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
ABUNDANCE
ALKALINE EARTH ISOTOPES
ALPHA REACTIONS
BARYON REACTIONS
BETA DECAY RADIOISOTOPES
BETA-PLUS DECAY RADIOISOTOPES
BINARY STARS
CALCIUM 40 TARGET
CHARGED-PARTICLE REACTIONS
CHROMIUM 46
CHROMIUM ISOTOPES
COPPER 58
COPPER ISOTOPES
COSMIC RADIO SOURCES
DAYS LIVING RADIOISOTOPES
ELECTRON CAPTURE RADIOISOTOPES
ELECTRON NEUTRINOS
ELECTRONS
ELEMENTARY PARTICLES
ERUPTIVE VARIABLE STARS
EVEN-EVEN NUCLEI
EXPLOSIONS
FERMIONS
FLUORINE 17 TARGET
FREEZING OUT
HADRON REACTIONS
HOURS LIVING RADIOISOTOPES
INTERMEDIATE MASS NUCLEI
ISOTOPES
KINETICS
LEPTONS
LIGHT NUCLEI
MAGNESIUM 24
MAGNESIUM ISOTOPES
MASSLESS PARTICLES
MILLISECONDS LIVING RADIOISOTOPES
MINUTES LIVING RADIOISOTOPES
NEON 20
NEON ISOTOPES
NEUTRINOS
NICKEL 56
NICKEL 57 TARGET
NICKEL ISOTOPES
NUCLEAR REACTIONS
NUCLEI
NUCLEON REACTIONS
NUCLEOSYNTHESIS
ODD-EVEN NUCLEI
ODD-ODD NUCLEI
PROTON REACTIONS
RADIOISOTOPES
REACTION KINETICS
SCANDIUM 41
SCANDIUM 43
SCANDIUM ISOTOPES
SECONDS LIVING RADIOISOTOPES
SEPARATION PROCESSES
SODIUM 21 TARGET
STABLE ISOTOPES
STARS
SUPERNOVA REMNANTS
SUPERNOVAE
SYNTHESIS
TARGETS
TITANIUM 42
TITANIUM 44
TITANIUM ISOTOPES
TWO-DIMENSIONAL CALCULATIONS
VANADIUM 45
VANADIUM 47
VANADIUM ISOTOPES
VARIABLE STARS
YEARS LIVING RADIOISOTOPES