The $^{22}$Ne(α,γ)$^{26}$Mg and $^{22}$Ne(α,n)$^{25}$Mg reactions play an important role in astrophysics because they have significant influence on the neutron flux during the weak branch of the s-process. We constrain the astrophysical rates for these reactions by measuring partial α-widths of resonances in $^{26}$Mg located in the Gamow window for the capture. These resonances were populated using $^{22}$Ne($^{6}$Li,d)$^{26}$Mg and $^{22}$Ne($^{7}$Li,t)$^{26}$Mg reactions at energies near the Coulomb barrier. At these low energies α-transfer reactions favor population of low spin states and the extracted partial α-widths for the observed resonances exhibit only minor dependence on the model parameters. The astrophysical rates for both the $^{22}$Ne(α,γ)$^{26}$Mg and the $^{22}$Ne(α,n)$^{25}$Mg reactions are shown to be significantly different than the previously suggested values.
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"value": "The $^{22}$Ne(\u03b1,\u03b3)$^{26}$Mg and $^{22}$Ne(\u03b1,n)$^{25}$Mg reactions play an important role in astrophysics because they have significant influence on the neutron flux during the weak branch of the s-process. We constrain the astrophysical rates for these reactions by measuring partial \u03b1-widths of resonances in $^{26}$Mg located in the Gamow window for the <math><mmultiscripts><mrow><mi>Ne</mi></mrow><mprescripts></mprescripts><none></none><mrow><mn>22</mn></mrow></mmultiscripts><mo>+</mo><mi>\u03b1</mi></math> capture. These resonances were populated using $^{22}$Ne($^{6}$Li,d)$^{26}$Mg and $^{22}$Ne($^{7}$Li,t)$^{26}$Mg reactions at energies near the Coulomb barrier. At these low energies \u03b1-transfer reactions favor population of low spin states and the extracted partial \u03b1-widths for the observed resonances exhibit only minor dependence on the model parameters. The astrophysical rates for both the $^{22}$Ne(\u03b1,\u03b3)$^{26}$Mg and the $^{22}$Ne(\u03b1,n)$^{25}$Mg reactions are shown to be significantly different than the previously suggested values."
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