Reaction rate sensitivity of 44Ti production in massive stars and implications of a thick target yield measurement for 40Ca(alpha,gamma)44Ti

R. D. Hoffman, S. A. Sheets, J. T. Burke, N. D. Scielzo, T. Rauscher

Research output: Chapter in Book/Report/Conference proceedingConference contribution

137 Downloads (Pure)

Abstract

The dynamic synergy between observation, theory, and experiment developed over many years around the field of gamma-ray astronomy has as its ultimate goal observations of specific radionuclides informing our understanding of stellar explosions and the theoretical models that predict nucleosynthesis. Observations of 56,57Ni and their decay products 56,57Co are used in many ways to constrain our current models of the core collapse mechanism. The radionuclide
44Ti (tau1/2 = 58.9 +- 0.3 yr), made in the same explosive environment but in much lower amounts compared to the very abundant nickel isotopes, is hoped to one day serve as an even more sensitive diagnostic and a valuable probe to the conditions extant in some of the deepest layers to be ejected. We [1] investigate 44Ti nucleosynthesis in adiabatic expansions from peak conditions drawn from a model for Cassiopia A and determine variations due to experimental
uncertainties in two key reaction rates. We find that the current uncertainty in these two rates could lead to as large a variation in 44Ti synthesis as that produced by different treatments of stellar physics in historical models of SNII.
Original languageEnglish
Title of host publicationProcs 11th Symposium on Nuclei in the Cosmos (NIC XI)
PublisherSISSA
Pages240
Number of pages5
Publication statusPublished - Jan 2011
Event11th Symposium on Nuclei in the Cosmos - Heidelberg, Germany
Duration: 19 Jul 201023 Jul 2010

Publication series

NameProceedings of Science
ISSN (Electronic)1824-8039

Conference

Conference11th Symposium on Nuclei in the Cosmos
Country/TerritoryGermany
CityHeidelberg
Period19/07/1023/07/10

Fingerprint

Dive into the research topics of 'Reaction rate sensitivity of 44Ti production in massive stars and implications of a thick target yield measurement for 40Ca(alpha,gamma)44Ti'. Together they form a unique fingerprint.

Cite this