Speaker
Dr
Alison Laird
(University of York)
Description
While core collapse supernovae have long captured the attention of
physicists and astronomers, surprisingly little is currently known about
the nature of the explosion mechanism. This is due to the complexity of
the explosion, the large computational requirements for even 2D
simulations, and the lack of precise nuclear physics inputs to these
models. One of the few methods by which this explosion mechanism might
be studied is through a comparison of the amount of 44Ti observed by
space based γ-ray telescopes and the amount predicted to have been generated
during the explosion. For these comparisons between observations and
models to be made, however, more precise nuclear physics inputs are
required. The reaction 21Na(α,p)24Mg has been identified as one of the
key reactions affecting the 44Ti mass fraction by factors of 10 or more.
There are currently no published data on this reaction.
A direct experimental measurement of the 21Na(α,p)24Mg cross section has been carried out at TRIUMF, Canada. This experiment utilised the TUDA facility at ISAC-I. The 21Na radioactive beam, at high intensity, impinged on a 2cm wide gas target, containing 100 torr of 4He. A downstream silicon array, consisting of a dE-E telescope,
detected the reaction protons. An upstream silicon array measured beam back-scattered from a Au foil located at the entrance of the gas target, for normalisation. Data were collected at four laboratory energies covering Ecm=3.2-2.5 MeV, which is approximately the top half of the 2GK Gamow Window. Preliminary analysis results will be presented, along with details of the experimental challenges encountered and the steps taken to overcome them.
Primary authors
Dr
Alison Laird
(University of York)
Dr
Simon Fox
(University of York)
