arXiv subjects

G. Staudt

Publications and source records attributed to G. Staudt.

14 recordsLinked to original sources

arXiv2002

The $^{15}$N($\bmα$,$\bmγ$)$^{19}$F reaction and nucleosynthesis of $^{19}$F

Several resonances in the $^{15}$N($α$,$γ$)$^{19}$F reaction have been investigated in the energy range between 0.6 MeV and 2.7 MeV. Resonance strengths and branching ratios have been determined. High sensitivity could be obtained by the combination of the {\sc{dynamitron}} high current accelerator, the windowless gas target system {\sc{rhinoceros}}, and actively shielded germanium detectors. Two levels of $^{19}$F could be observed for the first time in the ($α$,$γ$) channel, and several weak branchings below the detection limits of previous experiments were measured. Two observed resonances correspond to $α$-cluster states in $^{19}$F which have been assigned unambiguously. The astrophysical reaction rate is derived from this set of resonance strengths.

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arXiv2001

$^{92}$Mo($α,α$)$^{92}$Mo scattering,the $^{92}$Mo--$α$ optical potential, and the $^{96}$Ru($γ,α$)$^{92}$Mo reaction rate at astrophysically relevant energies

The elastic scattering cross section of$^{92}$Mo($α$,$α$)$^{92}$Mo has been measured at energies of $E_{\rm{c.m.}} \approx$ 13, 16, and 19 MeV in a wide angular range. The real and imaginary parts of the optical potential for the system $^{92}$Mo - $α$ have been derived at energies around and below the Coulomb barrier. The result fits into the systematic behavior of $α$-nucleus folding potentials. The astrophysically relevant $^{96}$Ru($γ$,$α$)$^{92}$Mo reaction rates at $T_9=2.0$ and $T_9=3.0$ could be determined to an accuracy of about 16 % and are compared to previously published theoretical rates.

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arXiv1998

Neutron capture of 26Mg at thermonuclear energies

The neutron capture cross section of 26Mg was measured relative to the known gold cross section at thermonuclear energies using the fast cyclic activation technique. The experiment was performed at the 3.75 MV Van-de-Graaff accelerator, Forschungszentrum Karlsruhe. The experimental capture cross section is the sum of resonant and direct contributions. For the resonance at E(n,lab) = 220 keV our new results are in disagreement with the data from Weigmann et al. An improved Maxwellian averaged capture cross section is derived from the new experimental data taking into account s- and p-wave capture and resonant contributions. The properties of so-called potential resonances which influence the p-wave neutron capture of 26}Mg are discussed in detail.

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arXiv1997

Direct neutron capture of 48Ca at kT = 52 keV

The neutron capture cross section of 48Ca was measured relative to the known gold cross section at kT = 52 keV using the fast cyclic activation technique. The experiment was performed at the Van-de-Graaff accelerator, Universitaet Tuebingen. The new experimental result is in good agreement with a calculation using the direct capture model. The 1/v behaviour of the capture cross section at thermonuclear energies is confirmed, and the adopted reaction rate which is based on several previous experimental investigations remains unchanged.

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arXiv1997

Comparison of low--energy resonances in 15N(alpha,gamma)19F and 15O(alpha,gamma)19Ne and related uncertainties

A disagreement between two determinations of Gamma_alpha of the astro- physically relevant level at E_x=4.378 MeV in 19F has been stated in two recent papers by Wilmes et al. and de Oliveira et al. In this work the uncertainties of both papers are discussed in detail, and we adopt the value Gamma_alpha=(1.5^{+1.5}_{-0.8})10^-9eV for the 4.378 MeV state. In addition, the validity and the uncertainties of the usual approximations for mirror nuclei Gamma_gamma(19F) approx Gamma_gamma(19Ne), theta^2_alpha(19F) approx theta^2_alpha(19Ne) are discussed, together with the resulting uncertainties on the resonance strengths in 19Ne and on the 15O(alpha,gamma)19Ne rate.

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arXiv1996

The ^{144}Sm-αoptical potential at astrophysically relevant energies derived from ^{144}Sm(α,α)^{144}Sm elastic scattering

For the determination of the $^{144}Sm-α$ optical potential we measured the angular distribution of $^{144}Sm(α,α)^{144}Sm$ scattering at the energy $E_{lab} = 20 MeV$ with high accuracy. Using the known systematics of $α$-nucleus optical potentials we are able to derive the $^{144}Sm-α$ optical potential at the astrophysically relevant energy $E_{c.m.} = 9.5 MeV$ with very limited uncertainties.

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arXiv1994

Direct mechanism in solar nuclear reactions

A short overview of the direct reaction mechanism and the models used for the analysis of such processes is given. Nuclear reactions proceeding through the direct mechanism and involved in solar hydrogen burning are discussed. The significance of these nuclear reactions with respect to the solar neutrino problem is investigated.

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arXiv1994

Direct mechanism in solar nuclear reactions

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arXiv1994

Systematics of $α$--nucleus optical potentials

Double--folded optical $α$--nucleus potentials can be used to calculate elastic scattering cross sections in a wide mass-- and energy region. Because of the systematic behavior of the potential parameters we are able to obtain reliable optical potentials for astrophysically relevant reactions even without scattering data in low--energy region. As example we analyze the capture reaction ${^{144}{\rm Sm}}(α,γ){^{148}{\Gd}}$.

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arXiv1994

Direct Capture at Low Energies

The importance of direct capture for (n,$γ$)--reactions on intermediate-- and heavy--mass target nuclei occuring in the s-- and r--process is investigated. It is shown that the direct mechanism is non--negligible for magic and neutron rich target nuclei. For some double magic and neutron rich nuclei in the r--process direct capture is even the dominant reaction mechanism.

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arXiv1993

Properties of $^{8}$Be and $^{12}$C deduced from the folding--potential model

The $α$--$α$ differential cross sections are analyzed in the optical model using a double--folded potential. With the knowledge of this potential bound and resonance--state properties of $α$--cluster states in $^{8}$Be and $^{12}$C as well as astrophysical S--factors of $^{4}$He($α$,$γ$)$^{8}$Be and $^{8}$Be($α$,$γ$)$^{12}$C are calculated. $Γ_γ$--widths and B(E2)--values are deduced.

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arXiv1993

Alpha Clustering and the stellar nucleosynthesis of carbon

The astrophysical S--factor and reaction rates for the triple--alpha process are calculated in the direct--capture model. It is shown that the stellar carbon production is extremely sensitive to small variations in the N--N interaction.

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arXiv1993

Properties of $^{8}$Be and $^{12}$C deduced from the folding--potential model

astro-ph↗

arXiv1993

Alpha scattering and capture reactions in the A = 7 system at low energies

Differential cross sections for $^3$He-$α$ scattering were measured in the energy range up to 3 MeV. These data together with other available experimental results for $^3$He $+ α$ and $^3$H $+ α$ scattering were analyzed in the framework of the optical model using double-folded potentials. The optical potentials obtained were used to calculate the astrophysical S-factors of the capture reactions $^3$He$(α,γ)^7$Be and $^3$H$(α,γ)^7$Li, and the branching ratios for the transitions into the two final $^7$Be and $^7$Li bound states, respectively. For $^3$He$(α,γ)^7$Be excellent agreement between calculated and experimental data is obtained. For $^3$H$(α,γ)^7$Li a $S(0)$ value has been found which is a factor of about 1.5 larger than the adopted value. For both capture reactions a similar branching ratio of $R = σ(γ_1)/σ(γ_0) \approx 0.43$ has been obtained.

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