C Vockenhuber et al 2008 J. Phys. G: Nucl. Part. Phys. 35 014034 doi:10.1088/0954-3899/35/1/014034
C Vockenhuber1, C O Ouellet2, L-S The3, L Buchmann1, J Caggiano1, A A Chen2, J M D'Auria4, B Davids1, L Fogarty1, D Frekers5, A Hussein6, D A Hutcheon1, W Kutschera7, D Ottewell1, M Paul8, M M Pavan1, J Pearson2, C Ruiz1, G Ruprecht1, M Trinczek1 and A Wallner7
Show affiliationsThe nuclide 44Ti is predicted to be produced in significant quantities in core-collapse supernovae, and indeed it has been observed in the supernova remnant Cassiopeia-A by space-based γ-ray telescopes. The main production of 44Ti takes place in the α-rich freeze-out phase deep inside the supernova. The key reactions governing the 44Ti abundance have been identified in an earlier sensitivity study. Using the recoil mass spectrometer DRAGON at the TRIUMF-ISAC facility in Vancouver, Canada, we measured the main production reaction 40Ca(α,γ)44Ti, resulting in an increased reaction rate compared to the rate derived from previous prompt γ-ray studies, which is commonly used in supernova models. The uncertainty of the 44Ti production is now dominated by the rate of reactions with short-lived nuclides around 44Ti, namely 45V(p,γ)46Cr, 44Ti(α,p)47V and 44Ti(α,γ)48Cr. The sensitivity of these reactions on the 44Ti production has been revisited.
25.55.-e 3H-, 3He-, and 4He-induced reactions
95.55.Ka X- and &ggr;-ray telescopes and instrumentation
27.40.+z 39(less-than-or-equal-to)A(less-than-or-equal-to)58
Issue 1 (January 2008)
Received 13 August 2007
Published 13 December 2007
C Vockenhuber et al 2008 J. Phys. G: Nucl. Part. Phys. 35 014034
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