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H. Oberhummer

Publications and source records attributed to H. Oberhummer.

At least 55 records · Page 3Linked to original sources

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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Astrophysically Relevant Neutron Capture near the Border of Stability

The neutron capture cross section on $^{26}$Mg was measured in the astrophysically relevant energy region from 25 keV to 220 keV. The experimental results agree well with a calculation using the Direct Capture (DC) model together with systematic folding potentials. This experiment confirms for the $^{26}$Mg(n,$γ$)$^{27}$Mg reaction that the DC process is at least comparable to the Compound--Nucleus (CN) process. The reliability of DC calculations is discussed, and we present some ideas for future experiments which could reduce the theoretical uncertainties of DC calculations.

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Reaction Rates of neutron capture by Li- and Be-isotopes

Neutron capture by neutron-rich Li- and Be-isotopes plays a role in big--bang nucleosynthesis, especially in its inhomogeneous version and in the $α$--process occurring in supernovae. New reaction rates for $^{7,8}$Li(n,$γ$)$^{8,9}$Li and $^{9,10,11}$Be(n,$γ$)$^{10,11,12}$Be have been consistently calculated using direct capture for the nonresonant part and the Breit-Wigner formula for the resonant part. The spectroscopic factors, spin/parity assignments and excitation energies of the final bound and initial resonant states have been taken from existing experimental data whenever possible. For unstable nuclei where this information is not experimentally available the shell model was used to determine these quantities.

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Uncertainties In Direct Neutron Capture Calculations Due To Nuclear Structure Models

The prediction of cross sections for nuclei far off stability is crucial in the field of nuclear astrophysics. For spherical nuclei close to the dripline the statistical model (Hauser-Feshbach) approach is not applicable and direct contributions may dominate the cross sections. For neutron-rich, even-even Sn targets, we compare the resulting neutron capture cross sections when consistently taking the input for the direct capture calculations from three different microscopic models. The results underline the sensitivity of cross sections calculated in the direct model to nuclear structure models which can lead to high uncertainties when lacking experimental information.

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Neutron-induced nucleosynthesis

Neutron--induced nucleosynthesis plays an important role in astrophysical scenarios like in primordial nucleosynthesis in the early universe, in the s--process occurring in Red Giants, and in the $α$--rich freeze--out and r--process taking place in supernovae of type II. A review of the three important aspects of neutron--induced nucleosynthesis is given: astrophysical background, experimental methods and theoretical models for determining reaction cross sections and reaction rates at thermonuclear energies. Three specific examples of neutron capture at thermal and thermonuclear energies are discussed in some detail.

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Measurement of neutron capture on $^{48}$Ca at thermal and thermonuclear energies

At the Karlsruhe pulsed 3.75\,MV Van de Graaff accelerator the thermonuclear $^{48}$Ca(n,$γ$)$^{49}$Ca(8.72\,min) cross section was measured by the fast cyclic activation technique via the 3084.5\,keV $γ$-ray line of the $^{49}$Ca-decay. Samples of CaCO$_3$ enriched in $^{48}$Ca by 77.87\,\% were irradiated between two gold foils which served as capture standards. The capture cross-section was measured at the neutron energies 25, 151, 176, and 218\,keV, respectively. Additionally, the thermal capture cross-section was measured at the reactor BR1 in Mol, Belgium, via the prompt and decay $γ$-ray lines using the same target material. The $^{48}$Ca(n,$γ$)$^{49}$Ca cross-section in the thermonuclear and thermal energy range has been calculated using the direct-capture model combined with folding potentials. The potential strengths are adjusted to the scattering length and the binding energies of the final states in $^{49}$Ca. The small coherent elastic cross section of $^{48}$Ca+n is explained through the nuclear Ramsauer effect. Spectroscopic factors of $^{49}$Ca have been extracted from the thermal capture cross-section with better accuracy than from a recent (d,p) experiment. Within the uncertainties both results are in agreement. The non-resonant thermal and thermonuclear experimental data for this reaction can be reproduced using the direct-capture model. A possible interference with a resonant contribution is discussed. The neutron spectroscopic factors of $^{49}$Ca determined from shell-model calculations are compared with the values extracted from the experimental cross sections for $^{48}$Ca(d,p)$^{49}$Ca and $^{48}$Ca(n,$γ$)$^{49}$Ca.

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Ground--state energies and widths of $^5$He and $^5$Li

We extract energies and widths of the ground states of $^5$He and $^5$Li from recent single--level R--matrix fits to the spectra of the $^3$H$({\rm d},γ$)$^5$He and the $^3$He$({\rm d},γ$)$^5$Li reactions. The widths obtained differ significantly from the formal R--matrix values but they are close to those measured as full widths at half maxima of the spectra in various experiments. The energies are somewhat lower than those given by usual estimates of the peak positions. The extracted values are close to the S--matrix poles calculated previously from the multi--term analyses of the N-$^4$He elastic scattering data.

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Reaction rate for two--neutron capture by $^4$He

Recent investigations suggest that the neutrino--heated hot bubble between the nascent neutron star and the overlying stellar mantle of a type--II supernova may be the site of the r--process. In the preceding $α$--process building up the elements to $A \approx 100$, the $^4$He(2n,$γ$)$^6$He-- and $^6$He($α$,n)$^9$Be--reactions bridging the instability gap at $A=5$ and $A=8$ could be of relevance. We suggest a mechanism for $^4$He(2n,$γ$)$^6$He and calculate the reaction rate within the $α$+n+n approach. The value obtained is about a factor 1.6 smaller than the one obtained recently in the simpler direct--capture model, but is at least three order of magnitude enhanced compared to the previously adopted value. Our calculation confirms the result of the direct--capture calculation that under representative conditions in the $α$--process the reaction path proceeding through $^6$He is negligible compared to $^4$He($α$n,$γ$)$^9$Be.

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Direct Neutron Capture for Magic-Shell Nuclei

In neutron capture for magic--shell nuclei the direct reaction mechanism can be important and may even dominate. As an example we investigated the reaction $^{48}$Ca(n,$γ)^{49}$Ca for projectile energies below 250\,keV in a direct capture model using the folding procedure for optical and bound state potentials. The obtained theoretical cross sections are in agreement with the experimental data showing the dominance of the direct reaction mechanism in this case. The above method was also used to calculate the cross section for $^{50}$Ca(n,$γ)^{51}$Ca.

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Cross section of $^{36}S(n,γ)^{37}S$

At the Karlsruhe pulsed 3.75 MV Van de Graaff accelerator the $^{36}S(n,γ)^{37}S(5.05 min)$ cross section was measured by the fast cyclic activation technique via the 3.103 MeV $γ$-ray line of the $^{37}$S-decay. Samples of elemental sulfur enriched in $^{36}$S by 5.933 % were irradiated between two gold foils which served as capture standards. The capture cross section was measured at the neutron energies 25, 151, 176, and 218 keV, respectively. The $^{36}S(n,γ)^{37}S$-cross section in the thermonuclear and thermal energy range has been calculated using the direct-capture (DC) model combined with the folding procedure used for the determination of the potentials. The non-resonant experimental data for this reaction can be reproduced excellently using this method. The input parameters of the DC-calculation (masses, Q-values, nuclear density distributions, spectroscopic factors, spin-parity assignments and excitation energies of the low-lying states of the residual nucleus) have been taken from the available experimental data.

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Nuclear Reactions of Astrophysical Interest Involving Light Nuclei

An introduction to nucleosynthesis, the creation of the elements in the big bang, in interstellar matter and in stars is given. The two--step process $^4$He(2n,$γ$)$^6$He and the reverse photodisintegration $^6$He($γ$,2n)$^4$He involving the halo nucleus $^6$He could be of importance in the $α$--process in type--II supernovae. The reaction rates for the above processes are calculated using three--body methods and show an enhancement of more than three orders of magnitude compared to the previous adopted value. Direct--capture calculations give similar values for the above reaction rates. Therefore, this method was also used to calculate the reaction rates of the two--step processes $^6$He(2n,$γ$)$^8$He and $^9$Li(2n,$γ$)$^{11}$Li and the reverse photodisintegration of $^8$He and $^{11}$Li that could be also of importance in the $α$-process.

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Searching for three-nucleon resonances

We search for three-neutron resonances which were predicted from pion double charge exchange experiments on He-3. All partial waves up to J=5/2 are nonresonant except the J=3/2^+ one, where we find a state at E=14 MeV energy with 13 MeV width. The parameters of the mirror state in the three-proton system are E=15 MeV and Gamma=14 MeV. The possible existence of an excited state in the triton, which was predicted from a H(He-6,alpha) experiment, is also discussed.

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Spectroscopic Amplitudes for One--Nucleon Transfer Between 1p0f--Shell Nuclei

Spectroscopic amplitudes are calculated for one--nucleon transfer between low--lying, normal--parity states of nuclei in the lower part of the 1p$0\,$f--shell. Calculations are performed using shell--model wave functions obtained from the diagonalization procedure of a nuclear Hamiltonian in the space given by the complete set of states generated from the 1p$_{3/2}$, 1p$_{1/2}$, $0\,$f$_{7/2}$ and $0\,$f$_{5/2}$ orbits. The Hamiltonian contains one and two body interactions derived recently by Richter \etal. Sum rules for one--nucleon pick--up and stripping reactions are given. The selectivity in excitation of the final states induced by one--nucleon pick--up or stripping is discussed.

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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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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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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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