<p>Recent sensitivity studies have shown that nucleosynthesis in Core-collapse supernovae (CCSNe) is significantly influenced by the <InlineEquation ID="IEq16"> <EquationSource Format="TEX">$^{13}$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mn>13</mn> </mmultiscripts> </math></EquationSource> </InlineEquation>N(<InlineEquation ID="IEq17"> <EquationSource Format="TEX">$\alpha , p$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>α</mi> <mo>,</mo> <mi>p</mi> </mrow> </math></EquationSource> </InlineEquation>)<InlineEquation ID="IEq18"> <EquationSource Format="TEX">$^{16}$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mn>16</mn> </mmultiscripts> </math></EquationSource> </InlineEquation>O reaction rate. However, the reaction rate at stellar temperatures (up to 4 GK) remains poorly constrained, primarily due to the limited knowledge of the decay properties of relevant <InlineEquation ID="IEq19"> <EquationSource Format="TEX">$^{17}$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mn>17</mn> </mmultiscripts> </math></EquationSource> </InlineEquation>F resonances above the <InlineEquation ID="IEq20"> <EquationSource Format="TEX">$\alpha $</EquationSource> <EquationSource Format="MATHML"><math> <mi>α</mi> </math></EquationSource> </InlineEquation> threshold at 5.819 MeV. To improve these constraints, we performed the <InlineEquation ID="IEq21"> <EquationSource Format="TEX">$^{19}$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mn>19</mn> </mmultiscripts> </math></EquationSource> </InlineEquation>F(<InlineEquation ID="IEq22"> <EquationSource Format="TEX">$p, t)^{17}$</EquationSource> <EquationSource Format="MATHML"><math> <msup> <mrow> <mi>p</mi> <mo>,</mo> <mi>t</mi> <mo stretchy="false">)</mo> </mrow> <mn>17</mn> </msup> </math></EquationSource> </InlineEquation>F transfer reaction experiment aimed at refining the <InlineEquation ID="IEq23"> <EquationSource Format="TEX">$^{13}$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mn>13</mn> </mmultiscripts> </math></EquationSource> </InlineEquation>N(<InlineEquation ID="IEq24"> <EquationSource Format="TEX">$\alpha , p$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>α</mi> <mo>,</mo> <mi>p</mi> </mrow> </math></EquationSource> </InlineEquation>)<InlineEquation ID="IEq25"> <EquationSource Format="TEX">$^{16}$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mn>16</mn> </mmultiscripts> </math></EquationSource> </InlineEquation>O rate. The experiment was performed at the tandem accelerator facility of the Japan Atomic Energy Agency using 30.5-MeV proton beams incident on CaF<InlineEquation ID="IEq26"> <EquationSource Format="TEX">$_2$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mn>2</mn> <mrow /> </mmultiscripts> </math></EquationSource> </InlineEquation> targets backed with gold. Recoiling tritons from the <InlineEquation ID="IEq27"> <EquationSource Format="TEX">$^{19}$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mn>19</mn> </mmultiscripts> </math></EquationSource> </InlineEquation>F(<InlineEquation ID="IEq28"> <EquationSource Format="TEX">$p, t)^{17}$</EquationSource> <EquationSource Format="MATHML"><math> <msup> <mrow> <mi>p</mi> <mo>,</mo> <mi>t</mi> <mo stretchy="false">)</mo> </mrow> <mn>17</mn> </msup> </math></EquationSource> </InlineEquation>F reaction were detected with segmented silicon detector arrays. The triton energy spectra revealed several low-lying <InlineEquation ID="IEq29"> <EquationSource Format="TEX">$^{17}$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mn>17</mn> </mmultiscripts> </math></EquationSource> </InlineEquation>F states, and angular distributions were analyzed using finite-range Distorted Wave Born Approximation (DWBA) calculations with multiple optical-model parameter sets. Proton and <InlineEquation ID="IEq30"> <EquationSource Format="TEX">$\alpha $</EquationSource> <EquationSource Format="MATHML"><math> <mi>α</mi> </math></EquationSource> </InlineEquation> decay channels associated with specific <InlineEquation ID="IEq31"> <EquationSource Format="TEX">$^{17}$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mn>17</mn> </mmultiscripts> </math></EquationSource> </InlineEquation>F resonances were clearly identified, which will allow us to determine the branching ratios. The optimized optical potentials and measured decay yields will provide direct experimental constraints on the <InlineEquation ID="IEq32"> <EquationSource Format="TEX">$\alpha $</EquationSource> <EquationSource Format="MATHML"><math> <mi>α</mi> </math></EquationSource> </InlineEquation>- and proton-partial widths (<InlineEquation ID="IEq33"> <EquationSource Format="TEX">$\Gamma _\alpha $</EquationSource> <EquationSource Format="MATHML"><math> <msub> <mi mathvariant="normal">Γ</mi> <mi>α</mi> </msub> </math></EquationSource> </InlineEquation>, <InlineEquation ID="IEq34"> <EquationSource Format="TEX">$\Gamma _p$</EquationSource> <EquationSource Format="MATHML"><math> <msub> <mi mathvariant="normal">Γ</mi> <mi>p</mi> </msub> </math></EquationSource> </InlineEquation>) of <InlineEquation ID="IEq35"> <EquationSource Format="TEX">$^{17}$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mn>17</mn> </mmultiscripts> </math></EquationSource> </InlineEquation>F levels in the Gamow window (<InlineEquation ID="IEq36"> <EquationSource Format="TEX">$E_x$</EquationSource> <EquationSource Format="MATHML"><math> <msub> <mi>E</mi> <mi>x</mi> </msub> </math></EquationSource> </InlineEquation> = 6–9.5 MeV). The resulting resonance parameters will enable a more reliable determination of the <InlineEquation ID="IEq37"> <EquationSource Format="TEX">$^{13}$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mn>13</mn> </mmultiscripts> </math></EquationSource> </InlineEquation>N(<InlineEquation ID="IEq38"> <EquationSource Format="TEX">$\alpha , p$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>α</mi> <mo>,</mo> <mi>p</mi> </mrow> </math></EquationSource> </InlineEquation>)<InlineEquation ID="IEq39"> <EquationSource Format="TEX">$^{16}$</EquationSource> <EquationSource Format="MATHML"><math> <mmultiscripts> <mrow /> <mrow /> <mn>16</mn> </mmultiscripts> </math></EquationSource> </InlineEquation>O reaction rate, thereby reducing its current uncertainty in CCSNe nucleosynthesis models.</p>

Investigating the $^{13}$N($\alpha , p$)$^{16}$O reaction rates via the $^{19}$F(p, t)$^{17}$F reaction

期刊论文
发表日期：

2026年4月22日

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Sohyun Kim,
Kyungyuk Chae,
Chanhee Kim,
Sunghoon Ahn,
Soomi Cha,
Jungwoo Lee,
Minju Kim,
Zifeng Luo,
Masato Asai,
Kentaro Hirose,
Testuya K. Sato,
Hiroyuki Makii,
Katsuhisa Nishio,
Riccardo Orlandi,
James Smallcombe,
Fumi Suzaki,
Taiki Tanaka,
Yuta Ito,
Sunghan Bae,
Fulong Liu,
Hidetoshi Yamaguchi,
Shigeru Kubono,
Minjeong Choi,
Nicoleta M. Florea,
Daniel Tofan,
Gyoungmo Gu,
Cheolmin Ham,
Dong Geon Kim,
Minsik Kwag,
Geonhee Oh

摘要

Recent sensitivity studies have shown that nucleosynthesis in Core-collapse supernovae (CCSNe) is significantly influenced by the $^{13}$ $^{13}$ N( $\alpha , p$ $α, p$ ) $^{16}$ $^{16}$ O reaction rate. However, the reaction rate at stellar temperatures (up to 4 GK) remains poorly constrained, primarily due to the limited knowledge of the decay properties of relevant $^{17}$ $^{17}$ F resonances above the $\alpha $ $α$ threshold at 5.819 MeV. To improve these constraints, we performed the $^{19}$ $^{19}$ F( $p, t)^{17}$ ${p, t)}^{17}$ F transfer reaction experiment aimed at refining the $^{13}$ $^{13}$ N( $\alpha , p$ $α, p$ ) $^{16}$ $^{16}$ O rate. The experiment was performed at the tandem accelerator facility of the Japan Atomic Energy Agency using 30.5-MeV proton beams incident on CaF $_2$ $_{2}$ targets backed with gold. Recoiling tritons from the $^{19}$ $^{19}$ F( $p, t)^{17}$ ${p, t)}^{17}$ F reaction were detected with segmented silicon detector arrays. The triton energy spectra revealed several low-lying $^{17}$ $^{17}$ F states, and angular distributions were analyzed using finite-range Distorted Wave Born Approximation (DWBA) calculations with multiple optical-model parameter sets. Proton and $\alpha $ $α$ decay channels associated with specific $^{17}$ $^{17}$ F resonances were clearly identified, which will allow us to determine the branching ratios. The optimized optical potentials and measured decay yields will provide direct experimental constraints on the $\alpha $ $α$ - and proton-partial widths ( $\Gamma _\alpha $ $Γ_{α}$ , $\Gamma _p$ $Γ_{p}$ ) of $^{17}$ $^{17}$ F levels in the Gamow window ( $E_x$ $E_{x}$ = 6–9.5 MeV). The resulting resonance parameters will enable a more reliable determination of the $^{13}$ $^{13}$ N( $\alpha , p$ $α, p$ ) $^{16}$ $^{16}$ O reaction rate, thereby reducing its current uncertainty in CCSNe nucleosynthesis models.

Investigating the \(^{13}\)N(\(\alpha , p\))\(^{16}\)O reaction rates via the \(^{19}\)F(p, t)\(^{17}\)F reaction

摘要