Trends in 44Ti and 56Ni from core-collapse supernovae

Georgios Magkotsios, Francis Timmes, Aimee L. Hungerford, Christopher L. Fryer, Patrick Young, Michael Wiescher

Research output: Contribution to journalArticle

63 Citations (Scopus)

Abstract

We compare the yields of 44Ti and 56Ni 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 44Ti and 56Ni yields for different mass elements. The 44Ti and 56Ni 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 44Ti and 56Ni 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 44Ti and 56Ni abundance evolution. Reactions that affect all yields globally are the 3α, p(e-, υe)n and n(e+, υe)p. The rest of the reactions are ranked according to their degree of impact on the synthesis of 44Ti. The primary ones include 44Ti(α, p) 47V, 40Ca(α, γ)44Ti, 45V(p, γ)46Cr, 40Ca(α, p) 43Sc, 17F(α, p)20Ne, 21Na(α, p)24Mg, 41Sc(p, γ) 42Ti, 43Sc(p, γ)44Ti, 44Ti(p, γ)45V, and 57Ni(p, γ)58Cu, along with numerous weak reactions. Our analysis suggests that not all 44Ti need to be produced in an α-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 44Ti observed in supernova remnants.

Original languageEnglish (US)
Pages (from-to)66-95
Number of pages30
JournalAstrophysical Journal, Supplement Series
Volume191
Issue number1
DOIs
StatePublished - Nov 2010

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supernovae
trends
power law
trajectory
trajectories
profiles
Cassiopeia A
supernova remnants
nuclear fusion
nuclear reactions
reaction rate
explosions
trend
explosion
tendencies
reaction kinetics
thermodynamics
shock
timescale
expansion

Keywords

  • Abundances
  • Hydrodynamics
  • Nuclear reactions
  • Nucleosynthesis
  • Supernovae: general

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Trends in 44Ti and 56Ni from core-collapse supernovae. / Magkotsios, Georgios; Timmes, Francis; Hungerford, Aimee L.; Fryer, Christopher L.; Young, Patrick; Wiescher, Michael.

In: Astrophysical Journal, Supplement Series, Vol. 191, No. 1, 11.2010, p. 66-95.

Research output: Contribution to journalArticle

Magkotsios, Georgios ; Timmes, Francis ; Hungerford, Aimee L. ; Fryer, Christopher L. ; Young, Patrick ; Wiescher, Michael. / Trends in 44Ti and 56Ni from core-collapse supernovae. In: Astrophysical Journal, Supplement Series. 2010 ; Vol. 191, No. 1. pp. 66-95.
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AB - We compare the yields of 44Ti and 56Ni 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 44Ti and 56Ni yields for different mass elements. The 44Ti and 56Ni 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 44Ti and 56Ni 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 44Ti and 56Ni abundance evolution. Reactions that affect all yields globally are the 3α, p(e-, υe)n and n(e+, υe)p. The rest of the reactions are ranked according to their degree of impact on the synthesis of 44Ti. The primary ones include 44Ti(α, p) 47V, 40Ca(α, γ)44Ti, 45V(p, γ)46Cr, 40Ca(α, p) 43Sc, 17F(α, p)20Ne, 21Na(α, p)24Mg, 41Sc(p, γ) 42Ti, 43Sc(p, γ)44Ti, 44Ti(p, γ)45V, and 57Ni(p, γ)58Cu, along with numerous weak reactions. Our analysis suggests that not all 44Ti need to be produced in an α-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 44Ti observed in supernova remnants.

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