The Feasibility of direct measurement of the 44Ti(α, p)47V and 40Ca(α, p)43Sc reactions in forward kinematics at astrophysically relevant temperatures
The Feasibility of direct measurement of the 44Ti(α, p)47V and 40Ca(α, p)43Sc reactions in forward kinematics at astrophysically relevant temperatures
复制标题
天体物理相关温度下正向运动学中直接测量 44Ti(α, p)47V 和 40Ca(α, p)43Sc 反应的可行性
DOI：
10.1140/epja/i2014-14140-8
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
K. Zuber
中科院分区：
文献类型：
--
作者：
T. Al-Abdullah;S. Akhmadaliev;M. Ayranov;D. Bemmerer;R. Dressler;Z. Elekes;N. Kivel;K. Schmidt;D. Schumann;M. Sobiella;T. Stowasser;M.P. Takács;K. Zuber
Understanding the synthesis of radioactive {sup 44}Ti in the α-rich freeze-out following core-collapse supernovae may help to better interpret such explosive events. The γ-ray lines from the decay of {sup 44}Ti have been observed by space-based γ-ray telescopes from two supernova remnants. It is believed that the {sup 44}Ti(α, p){sup 47}V reaction dominates the destruction of {sup 44}Ti, while the {sup 40}Ca(α, p){sup 43}Sc reaction removes fuel from the main {sup 44}Ti production reaction {sup 40}Ca(α, γ){sup 44}Ti. Here we report on a possible technique to determine both reaction rates at astrophysically relevant energies in forward kinematics. The first reaction will be performed using a 1-10 MBq {sup 44}Ti target. Two important concerns are considered to make this study possible: The amount of stable Ti in the radioactive target, which will be prepared via spallation reactions at Paul Scherrer Institute (PSI), and the degree of radioactive contaminations in the experimental setup due to sputtered {sup 44}Ti atoms after intensive irradiations. Several online and offline measurements in parallel with Monte Carlo simulations were performed to investigate these issues. (orig.)
Understanding the synthesis of radioactive {sup 44}Ti in the α-rich freeze-out following core-collapse supernovae may help to better interpret such explosive events. The γ-ray lines from the decay of {sup 44}Ti have been observed by space-based γ-ray telescopes from two supernova remnants. It is believed that the {sup 44}Ti(α, p){sup 47}V reaction dominates the destruction of {sup 44}Ti, while the {sup 40}Ca(α, p){sup 43}Sc reaction removes fuel from the main {sup 44}Ti production reaction {sup 40}Ca(α, γ){sup 44}Ti. Here we report on a possible technique to determine both reaction rates at astrophysically relevant energies in forward kinematics. The first reaction will be performed using a 1-10 MBq {sup 44}Ti target. Two important concerns are considered to make this study possible: The amount of stable Ti in the radioactive target, which will be prepared via spallation reactions at Paul Scherrer Institute (PSI), and the degree of radioactive contaminations in the experimental setup due to sputtered {sup 44}Ti atoms after intensive irradiations. Several online and offline measurements in parallel with Monte Carlo simulations were performed to investigate these issues. (orig.)
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影响因子：
3.1
作者：
K. Schmidt;S. Akhmadaliev;M. Anders;D. Bemmerer;A. Caciolli;M. Dietz;Z. Elekes;A. Junghans;M. Menzel;R. Schwengner;A. Wagner;K. Zuber
通讯作者：
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DOI：
--
发表时间：
1999
期刊：
影响因子：
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作者：
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DOI：
10.1088/0067-0049/191/1/66
发表时间：
2010
期刊：
The Astrophysical Journal Supplement Series
影响因子：
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作者：
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影响因子：
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作者：
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DOI：
--
发表时间：
2007
期刊：
影响因子：
--
作者：
Jin He;A. Murphy
通讯作者：
A. Murphy