The Excited states of ^(88)Sr have been produced in the reaction ^(16)O(^(82)Se,4p6n)and studied using the in-beam γ spectroscopy techniques.Two high-spin level structures have been observed and established up to 8.5...The Excited states of ^(88)Sr have been produced in the reaction ^(16)O(^(82)Se,4p6n)and studied using the in-beam γ spectroscopy techniques.Two high-spin level structures have been observed and established up to 8.5 MeV and 7.9 MeV excitation energy,respectively.Based on the measurements of the directional correlations ofγ-rays de-exciting oriented states and anisotropic factors ofγ-rays,spin values of the excited states have been assigned up to the highest levels observed.展开更多
Proton resonant states in 22Mg have been investigated by the resonant elastic scattering of 21Na+p. The 21Na beam with a mean energy of 4.00 MeV/u was separated by the CNS radioactive ion beam separator(CRIB) and bomb...Proton resonant states in 22Mg have been investigated by the resonant elastic scattering of 21Na+p. The 21Na beam with a mean energy of 4.00 MeV/u was separated by the CNS radioactive ion beam separator(CRIB) and bombarded a thick(CH2)n target. The energy spectra of recoiled protons were measured at scattering angles of θcm ≈172° and 146°,respectively. A new state at 7.06 MeV has been observed clearly and another new one at 7.28 MeV is tentatively identified due to its low statistics. The proton resonant parameters were deduced from an R-matrix analysis of the differential cross section data. The astrophysical resonant reaction rate for the 18Ne(α,p)21Na reaction has been estimated,and it is about five times larger than that assumed before.展开更多
The first stars in the early Universe were formed about 400 million years after the big bang. Verification of the existence of these stars is important for our understanding of the evolution of the Universe[1]. It has...The first stars in the early Universe were formed about 400 million years after the big bang. Verification of the existence of these stars is important for our understanding of the evolution of the Universe[1]. It has been predicted that for Population-III stellar production yields, the abundances of odd-Z elements are remarkably deficient compared to their adjacent even-Z elements[2]. Astronomers are searching for long-lived, low mass stars with the unique nucleosynthetic pattern matching the predicted yields[3].展开更多
Nathans et al (1986 a,b) have cloned the human (Cau-casian) color vision pigment genes located on X-chro-mosome and analyzed the corresponding DNA structurein normal and color-blind individuals.Jorgensen etal (1990) h...Nathans et al (1986 a,b) have cloned the human (Cau-casian) color vision pigment genes located on X-chro-mosome and analyzed the corresponding DNA structurein normal and color-blind individuals.Jorgensen etal (1990) have done similar analysis of persons ofAfrican and Japanese ancestry in the U.S.and disco-vered a new allele of the ’red’ gene.We report展开更多
基金Supported by the National Natural Science Foundation of China under Grant Nos.19705011 and 19635030the Chinese Academy of Sciences,and RIKEN Radiation Laboratory。
文摘The Excited states of ^(88)Sr have been produced in the reaction ^(16)O(^(82)Se,4p6n)and studied using the in-beam γ spectroscopy techniques.Two high-spin level structures have been observed and established up to 8.5 MeV and 7.9 MeV excitation energy,respectively.Based on the measurements of the directional correlations ofγ-rays de-exciting oriented states and anisotropic factors ofγ-rays,spin values of the excited states have been assigned up to the highest levels observed.
基金Japanese Ministry of Education, Culture,Sports,and Technology,Japan(13440071,14740156)Grants-in-Aids for JSPS,Japan(1604055)
文摘Proton resonant states in 22Mg have been investigated by the resonant elastic scattering of 21Na+p. The 21Na beam with a mean energy of 4.00 MeV/u was separated by the CNS radioactive ion beam separator(CRIB) and bombarded a thick(CH2)n target. The energy spectra of recoiled protons were measured at scattering angles of θcm ≈172° and 146°,respectively. A new state at 7.06 MeV has been observed clearly and another new one at 7.28 MeV is tentatively identified due to its low statistics. The proton resonant parameters were deduced from an R-matrix analysis of the differential cross section data. The astrophysical resonant reaction rate for the 18Ne(α,p)21Na reaction has been estimated,and it is about five times larger than that assumed before.
文摘The first stars in the early Universe were formed about 400 million years after the big bang. Verification of the existence of these stars is important for our understanding of the evolution of the Universe[1]. It has been predicted that for Population-III stellar production yields, the abundances of odd-Z elements are remarkably deficient compared to their adjacent even-Z elements[2]. Astronomers are searching for long-lived, low mass stars with the unique nucleosynthetic pattern matching the predicted yields[3].
文摘Nathans et al (1986 a,b) have cloned the human (Cau-casian) color vision pigment genes located on X-chro-mosome and analyzed the corresponding DNA structurein normal and color-blind individuals.Jorgensen etal (1990) have done similar analysis of persons ofAfrican and Japanese ancestry in the U.S.and disco-vered a new allele of the ’red’ gene.We report
