Abstract
The gamma-ray lines from the decay of 44Ti have been observed by space-based gamma-ray telescopes from two supernova remnants. It is believed that the 44Ti(α, p)47V reaction dominates the destruction of 44Ti. This work presents a possible technique to determine its reaction rate in forward kinematics at astrophysically relevant energies. Several online and offline measurements in parallel with Monte Carlo simulations were performed to illustrate the feasibility of performing this reaction. The results will be discussed.
Highlights
Core-collapse supernovae are believed to enrich the interstellar medium with heavy elements
Trying to improve the reaction rate, we report here a study that investigates the feasibility of performing the 44Ti(α, p)47V reaction in forward kinematics using 44Ti as a target
Experimental Setup The experiment is planned to be performed using the 4He++ beam provided by the 3 MV Tandetron accelerator at Helmholtz-Zentrum Dresden-Rossendorf (HZDR)
Summary
Core-collapse supernovae are believed to enrich the interstellar medium with heavy elements. The remnant of Cassiopeia A supernova gives clear evidences about its production, where emitted γ−lines first from 44Ti → 44Sc at 67.9 and 78.4 keV, and to 44Ca at 1157 keV have been detected by INTEGRAL [2] ( BeppoSAX [3]) and COMPTEL telescopes [4] respectively. These observations are confirmed from the remnant of supernova SN1987A [5]. The reaction was studied in inverse kinmatics by Sonzogni et al [7].
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