Identification of analog states in the T=1/2 A=27 mirror system from low excitation energies to the region of hydrogen burning in the 26Alg ,m(p,γ)27Si reactions

The reactions 26Alg(p,γ)27Si and 26Alm(p,γ)27Si are important for influencing the galactic abundance of the cosmic γ-ray emitter 26Alg and for the excess abundance of 26Mg found in presolar grains, respectively. Precise excitation energies and spin assignments of states from the ground state to the region of astrophysical interest in 27Si, including the identification and pairing of key astrophysical resonances with analog states in the mirror nucleus 27Al, are reported using γ rays observed in the 12C + 16O fusion reaction. The detailed evolution of Coulomb energy differences between the states in 27Si and 27Al is explored, including the region above the astrophysical reaction thresholds

Decay of the key 92-keV resonance in the 25Mg(p,γ) reaction to the ground and isomeric states of the cosmic γ-ray emitter 26Al

The 92-keV resonance in the 25Mg(p,γ)26Al reaction plays a key role in the production of 26Al at astrophysical burning temperatures of ≈100 MK in the Mg-Al cycle. However, the state can decay to feed either the ground, 26gAl, or isomeric state, 26mAl. It is the ground state that is critical as the source of cosmic γ rays. It is therefore important to precisely determine the ground-state branching fraction f0 of this resonance. Here we report on the identification of four γ-ray transitions from the 92-keV resonance, and determine the spin of the state and its ground-state branching fraction f0=0.52(2)stat(6)syst. The f0 value is the most precise reported to date, and at the lower end of the range of previously adopted values, implying a lower production rate of 26gAl and its cosmic 1809-keV γ rays.peerReviewe

Key resonances in the P30(p,γ)S31 gateway reaction for the production of heavy elements in ONe novae

Material emitted as ejecta from ONe novae outbursts is observed to be rich in elements as heavy as Ca. The bottleneck for the synthesis of elements beyond sulphur is the P30(p,γ)S31 reaction. Its reaction rate is, however, not well determined due to uncertainties in the properties of key resonances in the burning regime. In the present study, gamma-ray transitions are reported for the first time from all key states in S31 relevant for the P30(p,γ)S31 reaction. The spins and parity of these resonances have been deduced, and energies have been measured with the highest precision to date. The uncertainty in the estimated P30(p,γ)S31 reaction rate has been drastically reduced. The rate using this new information is typically higher than previous estimates based on earlier experimental data, implying a higher flux of material processed to high-Z elements in novae, but it is in good agreement with predictions using the Hauser-Feshbach approach at higher burning temperatures

Level structure of S 31: From low excitation energies to the region of interest for hydrogen burning in novae through the P 30 (p, γ) S 31 reaction

Comprehensive measurements of the excitation energy and spin-parity assignments for states in S31 are presented, from the first excited state, up to energies relevant for the P30(p,γ)S31 reaction in ONe novae. This reaction rate strongly influences heavy element abundances in novae ejecta. States in S31 are paired with their P31 analogues using γ rays detected with the Gammasphere detector array following the Si28(He4, n) fusion-evaporation reaction. The evolution of mirror energy differences is explored and the results are compared with new shell-model calculations. The excellent agreement observed in this work between experimental data and shell-model calculations provides confidence in using computed estimates in situations where experimental data are unavailable

Ação de fitoreguladores no desenvolvimento de Chrysanthemum leucanthemum L.

Plants of Chrysanthemum leucanthemum grown in pots with soil under greenhouse conditions, were sprayed with growth regulators twice, in May and June, to study the development of the plants in October. Succinic acid-2,2-dimethylhydrazide (SADH) at concentrations of 1250, 2500 and 5000 ppm, (2-chloroethyl) trimethylammonium chloride (CCC) 2000 ppm, (2-chloroethyl) phosphonic acid (CEPA) 320 ppm, maleic hydrazide (MH;) 1000 ppm, gibberellic acid (GA) 50 and 100 ppm, indolylacetic acid (IAA) 100 ppm, and water as check treatment, were applied. MH 1000 ppm reduced the number of leaves and stems. SADH treatments reduced the shoot growth and the number of stems. Applications of IAA 100 ppm promoted the formation of higher number of leaves and stems in Chrysanthemum leucanthemum. It was seen that sprays with GA at a concentration of 100 ppm elongated shoots.Plantas ornamentais de Chrysanthemum leucanthemum, cultivadas em recipientes contendo solo como substrato, em condições de estufa, foram pulverizadas em maio e junho com reguladores de crescimento, com a finalidade de se verificar a ação dos mesmos no desenvolvimento das plantas, determinado em outubro. Aplicaram-se SADH nas concentrações de 1250, 2500 e 5000 ppm, CCC na dosagem de 2000 ppm, CEPA 320 ppm, MH 1000 ppm, GA 50 e 100 ppm, IAA 100 ppm e água como controle. Hidrazida maleica 1000 ppm reduziu o número de folhas e hastes formadas. Tratamentos com ácido succínico - 2,2-dimetilhidrazida diminuiram a altura do caule e o número de hastes das plantas. Aplicações de ácido indolilacético 100 ppm promoveram a formação de maior número de folhas e de hastes em Chrysanthemum. Pulverizações com ácido giberélico 100 ppm incrementaram a altura do caule da espécie estudada

Shape coexistence from lifetime and branching-ratio measurements in 68,70Ni

© 2016 The Author(s) Shape coexistence near closed-shell nuclei, whereby states associated with deformed shapes appear at relatively low excitation energy alongside spherical ones, is indicative of the rapid change in structure that can occur with the addition or removal of a few protons or neutrons. Near 68Ni (Z=28, N=40), the identification of shape coexistence hinges on hitherto undetermined transition rates to and from low-energy 0+ states. In 68,70Ni, new lifetimes and branching ratios have been measured. These data enable quantitative descriptions of the 0+ states through the deduced transition rates and serve as sensitive probes for characterizing their nuclear wave functions. The results are compared to, and consistent with, large-scale shell-model calculations which predict shape coexistence. With the firm identification of this phenomenon near 68Ni, shape coexistence is now observed in all currently accessible regions of the nuclear chart with closed proton shells and mid-shell neutrons

Structure of resonances in the Gamow burning window for the Al 25 (p,γ) Si 26 reaction in novae

A γ-ray spectroscopy study of excited states in Si26 has been performed by using the Mg24(3He,n) reaction at a beam energy of 10 MeV. In particular, states have been studied above the proton threshold relevant for burning in the Al25(p,γ)Si26 reaction in novae. This reaction influences the amount of Al26 injected into the interstellar medium by novae, which contributes to the overall flux of cosmic γ-ray emission from Al26 observed in satellite missions. The present results point strongly to the existence of a 0+ state at an excitation energy of 5890 keV lying within the Gamow burning window, which raises questions about the existence and properties of another, higher-lying state reported in previous experimental work. The existence of two such states within this excitation energy region cannot be understood within the framework of sd-shell-model calculations. © 2015 American Physical Society

Decay of the key 92-keV resonance in the 25Mg(p,γ) reaction to the ground and isomeric states of the cosmic γ-ray emitter 26Al

The 92-keV resonance in the 25Mg(p,γ)26Al reaction plays a key role in the production of 26Al at astrophysical burning temperatures of ≈100 MK in the Mg-Al cycle. However, the state can decay to feed either the ground, 26gAl, or isomeric state, 26mAl. It is the ground state that is critical as the source of cosmic γ rays. It is therefore important to precisely determine the ground-state branching fraction f0 of this resonance. Here we report on the identification of four γ-ray transitions from the 92-keV resonance, and determine the spin of the state and its ground-state branching fraction f0=0.52(2)stat(6)syst. The f0 value is the most precise reported to date, and at the lower end of the range of previously adopted values, implying a lower production rate of 26gAl and its cosmic 1809-keV γ rays

Revised decay properties of the key 93-keV resonance in the Mg 25 (p,γ) reaction and its influence on the MgAl cycle in astrophysical environments

The γ-decay properties of an excited state in Al26 at 6398.3(8) keV have been reexamined using the B11+O16 fusion-evaporation reaction. This level represents a key 93.1(8)-keV resonance in the Mg25+p system and its relative branching to the Al26 ground state, f0, has been determined to be 0.76±0.03 (stat.) ±0.10 (syst.). This is a significantly higher value than the most recent evaluation and implies a considerable increase in the production of cosmic γ rays from Al26 radioactivity

Identification of γ -decaying resonant states in 26Mg and their importance for the astrophysical s process

The 22Ne(α, n) reaction is expected to provide the dominant neutron source for the weak s process in massive stars and intermediate-mass (IM) Asymptotic Giant Branch (AGB) stars. However, the production of neutrons in such environments is hindered by the competing 22Ne(α,γ)26Mg reaction. Here, the 11B(16O,p) fusion-evaporation reaction was used to identify γ-decay transitions from 22Ne + α resonant states in 26Mg. Spin-parity restrictions have been placed on a number of α-unbound excited states in 26 Mg and their role in the 22Ne(α,γ)26Mg reaction has been investigated. In particular, a suspected natural-parity resonance at Ec.m. = 557(3) keV, that lies above the neutron threshold in 26Mg, and is known to exhibit a strong α-cluster character, was observed to γ decay. Furthermore, a known resonance at Ec . m .= 466 (4 ) keV has been definitively assigned 2+ spin and parity. Consequently, uncertainties in the 22Ne(α,γ) stellar reaction rate have been reduced by a factor of ∼ 20 for temperatures ∼ 0.2 GK