Study of the 44Ti(α, p)47V reaction and implications for core collapse supernovae

V. Margerin, A. Murphy, T. Davinson, R. Dressler, J. Fallis, A. Kankainen, A.M. Laird, G. Lotay, D.J. Mountford, C.D. Murphy, C. Seiffert, D. Schumann, T. Stowasser, T. Stora, C.H.-T. Wang, P.J. Woods

Research output: Contribution to journalArticlepeer-review

Abstract / Description of output

The underlying physics triggering core collapse supernovae is not fully understood but observations of material ejected during such events helps to solve this puzzle. In particular, several satellite based γ -ray observations of the isotope 44Ti have been reported recently. Conveniently, the amount of this
isotope in stellar ejecta is thought to depend critically on the explosion mechanism. The most influential reaction to the amount of 44Ti in supernovae is 44Ti(α, p)47V. Here we report on a direct study of this reaction conducted at the REX-ISOLDE facility, CERN. The experiment was performed with a 44Ti beam at Elab = 2.16 MeV/u, corresponding to an energy distribution, for reacting α-particles, centred on Ecm = 4.15 with a 1σ width of 0.23 MeV. This is, for the first time, well within the Gamow window for core collapse supernovae. The material from which the 44Ti beam was extracted originates from highly
irradiated components of the SINQ spallation neutron source of the Paul Scherrer Institute. No yield above background was observed, enabling an upper limit for the rate of this reaction to be determined. This result is below expectation, suggesting that the 44Ti(α, p)47V reaction proceeds more slowly than
previously thought. Implications for astrophysical events, and remnant age, are discussed.
Original languageEnglish
Pages (from-to)358-361
Number of pages4
JournalPhysics Letters B
Early online date12 Mar 2014
Publication statusE-pub ahead of print - 12 Mar 2014


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