No abstract available

[en] Nuclear properties of the excited states below 3.2 MeV in ⁵⁶Cr were studied in the ⁵⁴Cr(t, pγ)⁵⁶Cr reaction at E/sub t/ = 2.9 MeV. Reaction-produced protons were detected at 171degree +- 4degree to the beam in coincidence with γ rays. γ-ray angular correlations and branching ratios were measured using an array of five NaI(Tl) crystals, while γ-ray energies and lifetime limits were obtained using a Ge(Li) detector. Spin assignments for some of the excited states were obtained in addition to multipole mixing-ratio information. The results for the excitation energies (keV), spins, and lifetimes (psec) are: 1007.6 +- 1.5, 2, > or =2; 1832.2 +- 2.6, 2, undetermined; 2327.8 +- 2.6, 2, < or =0.08; 2687 +- 13, 1, 2, 3, or 4, undetermined; 3165.6 +- 6.2, 2, 3, or 4, < or =0.3. The results are compared with shell-model calculations

[en] Short note. 3 refs

[en] Emergence of α-clustering in nuclei and its impact on their various properties, particularly starting from light nuclei within the nuclear table remains a topic of contemporary interest. In this present work, we have populated the excited states in ⁵⁴Cr via the α-transfer to ⁵⁰Ti nucleus. The reactions were studied through particle-γ coincidence measurements. Our findings suggest moderate α-cluster structure for the yrast states of ⁵⁴Cr and the clustering effect reduces for the non-yrast states

[en] The proton induced reactions play important role as energy generating processes in different stages of evolution of stars. The seeds in the concerned mass region A=40-54 are mainly produced in hydrostatic carbon burning and explosive oxygen burning and they take part in initiating the rp-process nucleosynthesis. This ultimately results in thermal burst in some astrophysical scenario e.g. in x-ray bursters. Study of the nucleosynthesis mechanism during various phases of stellar burning requires a complicated and coupled network calculation concerning various reaction rates or cross sections. However, very often these rates can not be measured experimentally due to instability and unavailability of targets. In such cases, theoretical extrapolation can supplement the purpose

[en] Short note. 3 refs.; 1 tab

[en] Cross sections for production of individual γ rays in the ⁵⁴Cr(p,γ)⁵⁵Mn reaction have been measured over the proton energy range 1.0-3.8 MeV. Gamma-ray yeilds are observed to fall by factors of between 5 and 10 at the crossing of the neutron threshold for a proton bombarding energy of 2.2 MeV. Statistical model calculations with global parameter sets successfully account for the dramatic effect of neutron competition on the (p,γ) cross section, and at the same time correctly predict the ⁵⁴Cr(p,n)⁵⁴Mn reaction cross section

No abstract available

[en] Cross sections for production of individual γ-rays in the ⁵⁴Cr(p,γ)⁵⁵Mn reaction have been measured over the proton energy range 1.0 to 3.8 MeV. Gamma ray yields are observed to fall by factors of between 5 and 10 at the crossing of the neutron threshold at a proton bombarding energy of 2.2 MeV. Statistical model calculations with global parameter sets successfully account for the dramatic effect of neutron competition on the (p,γ) cross section, and at the same time correctly predict the ⁵⁴Cr (p,n)⁵⁴Mn reaction cross section

No abstract available