Nuclear astrophysics and AMS – Probing nucleosynthesis in the lab

Wallner, A.

doi:10.1016/j.nimb.2009.10.152

Cited by 39 publications

(37 citation statements)

References 53 publications

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“…The VERA facility AMS was introduced to laboratory experiments in nuclear astrophysics already in 1980 by Paul et al [32] with a first study of the 25 Mg(p,n) 26 Al reaction. In particular, the past few years have seen an increasing number of nuclear astrophysics measurements with the AMS technique for charged particle and neutron induced reactions (see, e.g., [33][34][35][36][37][38][39][40][41]). …”

Section: Accelerator Mass Spectrometrymentioning

confidence: 99%

Accelerator mass spectrometry measurements of theC13(n,γ)C14and
Wallner
¹
,
Bichler
²
,
Buczak
³

et al. 2016
Phys. Rev. C
28
1
17
0
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The technique of accelerator mass spectrometry (AMS), offering a complementary tool for sensitive studies of key reactions in nuclear astrophysics, was applied for measurements of the 13 C(n,γ ) 14 C and the 14 N(n,p) 14 C cross sections, which act as a neutron poison in s-process nucleosynthesis. Solid samples were irradiated at Karlsruhe Institute of Technology with neutrons closely resembling a Maxwell-Boltzmann distribution for kT = 25 keV, and also at higher energies between E n = 123 and 182 keV. After neutron irradiation the produced amount of 14 C in the samples was measured by AMS at the Vienna Environmental Research Accelerator (VERA) facility. For both reactions the present results provide important improvements compared to previous experimental data, which were strongly discordant in the astrophysically relevant energy range and missing for the comparably strong resonances above 100 keV. For 13 C(n,γ ) we find a four times smaller cross section around kT = 25 keV than a previous measurement. For 14 N(n,p), the present data suggest two times lower cross sections between 100 and 200 keV than had been obtained in previous experiments and data evaluations. The effect of the new stellar cross sections on the s process in low-mass asymptotic giant branch stars was studied for stellar models of 2 M initial mass, and solar and 1/10 th solar metallicity.

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Section: Accelerator Mass Spectrometrymentioning

confidence: 99%

Accelerator mass spectrometry measurements of theC13(n,γ)C14and
Wallner
¹
,
Bichler
²
,
Buczak
³

et al. 2016
Phys. Rev. C
28
1
17
0
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“…Platinum isotopes by AMS were performed at VERA, a 3 MV tandem accelerator at the University of Vienna, which has been designed for AMS measurements up to the heaviest nuclides (Steier et al 2005;Wallner 2010). Because of a high Pt background the original ion source SNICS (Kutschera et al 1997) was replaced for our measurements by a new source SN2 of identical design (Priller et al 2010).…”

Section: Ams Measurementsmentioning

confidence: 99%

New Attempts to Understand Nanodiamond Stardust

Ott

Besmehn

Farouqi

et al. 2012

Publ. Astron. Soc. Aust

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Abstract:We report on a concerted effort aimed at understanding the origin and history of the pre-solar nanodiamonds in meteorites including the astrophysical sources of the observed isotopic abundance signatures. This includes measurement of light elements by secondary ion mass spectrometry (SIMS), analysis of additional heavy trace elements by accelerator mass spectrometry (AMS) and dynamic calculations of r-process nucleosynthesis with updated nuclear properties. Results obtained indicate that: (i) there is no evidence for the former presence of now-extinct 26 Al and 44 Ti in our diamond samples other than what can be attributed to silicon carbide and other 'impurities', and this does not offer support for a supernova (SN) origin but neither does it negate it; (ii) analysis by AMS of platinum in 'bulk diamond' yields an overabundance of r-only 198 Pt that at face value seems more consistent with the neutron burst than with the separation model for the origin of heavy trace elements in the diamonds, although this conclusion is not firm given analytical uncertainties; (iii) if the Xe-H pattern was established by an unadulterated r-process, it must have been a strong variant of the main r-process, which possibly could also account for the new observations in platinum.

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“…But also charged-particle cross sections of astrophysical interest have been measured, e.g. the 25 Mg(p, γ) 26 Al g and 40 Ca(α, γ) 44 Ti cross sections [42,43]. An overview of cross sections measured with AMS for nuclear astrophysics so far is given in Refs.…”

Section: Au Cross Sectionmentioning

confidence: 99%

“…An overview of cross sections measured with AMS for nuclear astrophysics so far is given in Refs. [44] and [45].…”

Section: Au Cross Sectionmentioning

confidence: 99%

Measurement of the stellarNi58(n,γ)Ni59cross section with accelerator mass spectrometry

et al. 2017

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The 58 Ni(n, γ) 59 Ni cross section was measured with a combination of the activation technique and accelerator mass spectrometry (AMS). The neutron activations were performed at the Karlsruhe 3.7 MV Van de Graaff accelerator using the quasi-stellar neutron spectrum at kT = 25 keV produced by the 7 Li(p, n) 7 Be reaction. The subsequent AMS measurements were carried out at the 14 MV tandem accelerator of the Maier-Leibnitz-Laboratory in Garching using the Gas-filled Analyzing Magnet System (GAMS). Three individual samples were measured, yielding a Maxwellian-averaged cross section at kT = 30 keV of σ 30keV = 30.4 (23) syst (9) stat mbarn. This value is slightly lower than two recently published measurements using the time-of-flight (TOF) method, but agrees within the uncertainties. Our new results also resolve the large discrepancy between older TOF measurements and our previous value.

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Nuclear astrophysics and AMS – Probing nucleosynthesis in the lab

Cited by 39 publications

References 53 publications

Accelerator mass spectrometry measurements of theC13(n,γ)C14and
Wallner
¹
,
Bichler
²
,
Buczak
³

et al. 2016
Phys. Rev. C
28
1
17
0
View full text Add to dashboard Cite

Accelerator mass spectrometry measurements of theC13(n,γ)C14and
Wallner
¹
,
Bichler
²
,
Buczak
³

et al. 2016
Phys. Rev. C
28
1
17
0
View full text Add to dashboard Cite

New Attempts to Understand Nanodiamond Stardust

Measurement of the stellarNi58(n,γ)Ni59cross section with accelerator mass spectrometry

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Nuclear astrophysics and AMS – Probing nucleosynthesis in the lab

Cited by 39 publications

References 53 publications

Accelerator mass spectrometry measurements of theC13(n,γ)C14andWallner1, Bichler2, Buczak3 et al. 2016Phys. Rev. C281170View full textAdd to dashboardCite

Accelerator mass spectrometry measurements of theC13(n,γ)C14andWallner1, Bichler2, Buczak3 et al. 2016Phys. Rev. C281170View full textAdd to dashboardCite

New Attempts to Understand Nanodiamond Stardust

Measurement of the stellarNi58(n,γ)Ni59cross section with accelerator mass spectrometry

Contact Info

Product

Resources

About

Accelerator mass spectrometry measurements of theC13(n,γ)C14and
Wallner
¹
,
Bichler
²
,
Buczak
³

et al. 2016
Phys. Rev. C
28
1
17
0
View full text Add to dashboard Cite

Accelerator mass spectrometry measurements of theC13(n,γ)C14and
Wallner
¹
,
Bichler
²
,
Buczak
³

et al. 2016
Phys. Rev. C
28
1
17
0
View full text Add to dashboard Cite