Статья

<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>α</mml:mi></mml:math>Decay of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">I</mml:mi><mml:mprescripts/><mml:none/><mml:mn>109</mml:mn></mml:mmultiscripts></mml:math>and Its Implications for the Proton Decay of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi>Sb</mml:mi><mml:mprescripts/><mml:none/><mml:mn>105</mml:mn></mml:mmultiscripts></mml:math>and the Astrophysical Rapid Proton-Capture Process

C. MazzocchiDepartment of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USAR. GrzywaczDepartment of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USAS. N. LiddickUNIRIB, Oak Ridge Associated Universities, Oak Ridge, Tennessee 37831, USAK. P. RykaczewskiPhysics Division, Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USAH. SchatzNational Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USAJ. C. BatchelderUNIRIB, Oak Ridge Associated Universities, Oak Ridge, Tennessee 37831, USAC. R. BinghamDepartment of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USAC. J. GrossPhysics Division, Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USAJ. H. HamiltonDepartment of Physics and Astronomy, Vanderbilt University, Nashville, Tennessee 37235, USAJ. K. HwangDepartment of Physics and Astronomy, Vanderbilt University, Nashville, Tennessee 37235, USAS. IlyushkinDepartment of Physics and Astronomy, Mississippi State University, Mississippi 39762, USAA. KorgulDepartment of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USAW. KrólasInstitute of Nuclear Physics, Polish Academy of Sciences, PL 31-342 Kraków, PolandK. LiDepartment of Physics and Astronomy, Vanderbilt University, Nashville, Tennessee 37235, USAR. D. PageDepartment of Physics, University of Liverpool, Liverpool, L69 7ZE, United KingdomDelia M. SimpsonDepartment of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USAJ. A. WingerDepartment of Physics and Astronomy, Mississippi State University, Mississippi 39762, USA

2007lv

ABI

Аннотация

An $\ensuremath{\alpha}$-decay branch of $(1.4\ifmmode\pm\else\textpm\fi{}0.4)\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}4}$ has been discovered in the decay of $^{109}\mathrm{I}$, which predominantly decays via proton emission. The measured ${Q}_{\ensuremath{\alpha}}$ value of $3918\ifmmode\pm\else\textpm\fi{}21\text{ }\text{ }\mathrm{keV}$ allows the indirect determination of the $Q$ value for proton emission from $^{105}\mathrm{Sb}$ of $356\ifmmode\pm\else\textpm\fi{}22\text{ }\text{ }\mathrm{keV}$, which is approximately of 130 keV more bound than previously reported. This result is relevant for the astrophysical rapid proton-capture process, which would terminate in the $^{105}\mathrm{Sn}(p,\ensuremath{\gamma})^{106}\mathrm{Sb}(p,\ensuremath{\gamma})^{107}\mathrm{Te}(\ensuremath{\alpha}\mathrm{\text{decay}})^{103}\mathrm{Sn}$ cycle at the densities expected in explosive hydrogen burning scenarios, unless unusually strong pairing effects result in a $^{103}\mathrm{Sn}(p,\ensuremath{\gamma})^{104}\mathrm{Sb}(p,\ensuremath{\gamma})^{105}\mathrm{Te}(\ensuremath{\alpha}\mathrm{\text{decay}})^{101}\mathrm{Sn})$ cycle.

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Идентификаторы

DOI: 10.1103/physrevlett.98.212501

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Цитирований: 2Использованных источников: 0

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