Study of the $${{^{25}}}$$Mg(d,p)$${{^{26}}}$$Mg reaction to constrain the $${{^{25}}}$$Al(p,$${\gamma }$$)$${{^{26}}}$$Si resonant reaction rates in nova burning conditions

  title={Study of the \$\$\{\{^\{25\}\}\}\$\$Mg(d,p)\$\$\{\{^\{26\}\}\}\$\$Mg reaction to constrain the \$\$\{\{^\{25\}\}\}\$\$Al(p,\$\$\{\gamma \}\$\$)\$\$\{\{^\{26\}\}\}\$\$Si resonant reaction rates in nova burning conditions},
  author={C. B. Hamill and P. J. Woods and D. Kahl and Richard Longland and J. P. Greene and Caleb Marshall and F. Portillo and Kiana Setoodehnia},
  journal={European Physical Journal A},
The rate of the $$^{25}$$Al(p, $$\gamma $$)$$^{26}$$Si reaction is one of the few key remaining nuclear uncertainties required for predicting the production of the cosmic $$\gamma $$-ray emitter $$^{26}$$Al in explosive burning in novae. This reaction rate is dominated by three key resonances ($$J^{\pi }=0^{+}$$, $$1^{+}$$ and $$3^{+}$$) in $$^{26}$$Si. Only the $$3^{+}$$ resonance strength has been directly constrained by experiment. A high resolution measurement of the $$^{25}$$Mg(d, p… 
5 Citations

AMS cross-section measurement for the $$^{28}$$Si(d,$$\alpha $$)$$^{26}$$Al reaction near the Coulomb barrier

Understanding the production of $$^{26}$$ Al is important in nuclear physics, astrophysics (stellar nucleosynthesis), earth sciences and other fields. In previous years, we attempted to measure the

New constraints on the Al25(p,γ) reaction and its influence on the flux of cosmic γ rays from classical nova explosions

The astrophysical $^{25}\mathrm{Al}(p,\ensuremath{\gamma})\phantom{\rule{0.16em}{0ex}}^{26}\mathrm{Si}$ reaction represents one of the key remaining uncertainties in accurately modeling the abundance

Cluster transfer reactions with the combined R-matrix and Lagrange-mesh methods

We have recently applied the R -matrix method to transfer reactions in the distorted wave Born approximation (DWBA) framework. In our approach the wave function in the internal region is expanded in



Spectroscopy of positive parity states in 26Mg and 26Al via the ( alpha,3He) and ( alpha,t) reactions.

  • YasuèOgawa Hamada
  • Materials Science
    Physical review. C, Nuclear physics
  • 1990
The total observed strengths for neutron stripping to the positive-parity states in the region of ${\mathit{E}}_{\math it{x}}$=0--11 MeV almost attained the limit of the pure j-j coupling scheme.

Lowest l = 0 proton resonance in Si 26 and implications for nucleosynthesis of Al 26

Using a beam of the radioactive isotope $^{25}\mathrm{Al}$, produced with the new RESOLUT facility, we measured the direct $(d,n)$ proton-transfer reaction leading to low-lying proton resonances in

Astrophysically importantSi26states studied with the(He3,n)reaction and theAl25(p,γ)Si26reaction rates in explosive hydrogen burning environments

Additional experimental information concerning the level structure of {sup 26}Si above the proton threshold is needed to reduce uncertainties in the {sup 25}Al(p,{gamma}){sup 26}Si reaction rate and

A new study of 25Mg$(\alpha, n)$28Si angular distributions at $E_{\alpha} =3-5$ MeV

Abstract.The observation of 26Al gives us the proof of active nucleosynthesis in the Milky Way. However the identification of the main producers of 26Al is still a matter of debate. Many sites have

High-precision (p,t) reaction to determine Al-25(p,gamma)Si-26 reaction rates

Since the identification of ongoing Al-26 production in the universe, the reaction sequence Mg-24(p,gamma)Al-25(beta(+)nu)Mg-25(p,gamma)Al-26 has been studied intensively. At temperatures where the

Radioactive 26Al from massive stars in the Galaxy

High spectral resolution measurements of 26Al emission at 1808.65 keV demonstrate that the 26Al source regions corotate with the Galaxy, supporting its Galaxy-wide origin and determining a present-day equilibrium mass of 2.8 (± 0.8) solar masses of 27Al.

Spectroscopic factor of the 1 + , 25 Al(p,γ) 26 Si resonance at E x =5.68 MeV

Nuclear shell model predictions for the proton spectroscopic factor of the 1+, Ex = 5.68 MeV level in 26Si are about fifty times smaller than the value suggested by the measured (a,3He) cross section

Presolar grains from novae

We report the discovery of five SiC grains and one graphite grain isolated from the Murchison carbonaceous meteorite whose major-element isotopic compositions indicate an origin in nova explosions.

Excited states above the proton threshold in 26Si

The level scheme above the proton threshold in 26Si is crucial for evaluating the 25Al(p, γ)26Si stellar reaction, which is important for understanding the astrophysical origin of the long-lived