Applications of accelerator mass spectrometry

Kutschera, W.

doi:10.1016/j.ijms.2013.05.023

Cited by 94 publications

(76 citation statements)

References 238 publications

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“…Several approaches can be made to reduce isobaric interference, e.g. : specialised sample preparation can reduce the amount of the stable isobar; selecting either an elemental ion or a particular molecular ion can reduce the intensity of the isobar significantly; or spatial separation of isobars can be achieved in a gas-filled magnetic spectrograph [233,197,198,199]. By taking advantage of the different energy loss behaviour of different elements in dedicated particle detectors allows them to be distinguished in principle, AS the ions are identified by their position, energy, energy loss signals and their entering angle.…”

Section: Ams Techniquementioning

confidence: 99%

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The activation method for cross section measurements in nuclear astrophysics

et al. 2019

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The primary aim of experimental nuclear astrophysics is to determine the rates of nuclear reactions taking place in stars in various astrophysical conditions. These reaction rates are important ingredient for understanding the elemental abundance distribution in our solar system and the galaxy. The reaction rates are determined from the cross sections which need to be measured at energies as close to the astrophysically relevant ones as possible. In many cases the final nucleus of an astrophysically important reaction is radioactive which allows the cross section to be determined based on the off-line measurement of the number of produced isotopes. In general, this technique is referred to as the activation method, which often has substantial advantages over in-beam particle-or γ-detection measurements. In this paper the activation method is reviewed from the viewpoint of nuclear astrophysics. Important aspects of the activation method are given through several reaction studies for charged particle, neutron and γ-induced reactions. Various techniques for the measurement of the produced activity are detailed. As a special case of activation, the technique of Accelerator Mass Spectrometry in cross section measurements is also reviewed. PACS. 26.20.-f Hydrostatic stellar nucleosynthesis -26.30.-k Nucleosynthesis in novae, supernovae, and other explosive environments -24.10.-i Nuclear reaction models and methodsContents

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Section: Ams Techniquementioning

confidence: 99%

“…AMS is a single-atom counting technique, usually used to measure minute amounts of nuclides in mg-sized samples. AMS represents the most sensitive technique for quantifying long-lived radionuclides [197,198,199]. It is a mass spectrometric technique based on the use of a (tandem) accelerator.…”

Section: Introductionmentioning

confidence: 99%

The activation method for cross section measurements in nuclear astrophysics

et al. 2019

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“…5. Accelerator Mass Spectrometry (AMS) [37,38] is an ultra-sensitive and ultra-selective analytical method for the detection of trace amounts (sub-ng range) of longlived radioactive isotopes like 59 Ni. AMS allows the determination of the concentration of the radioisotope relative to the ion current of a stable isotope (ideally of the same element).…”

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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“…Atomic stable isobars, which are much more abundant in nature than the corresponding isobaric radionuclide, will pass through the AMS setup in the same manner, and will be suppressed by specific methods for different elements. Therefore, AMS is highly sensitive and capable of quantifying very small isotopic ratios as low as 10 −16 , which makes it very suitable for a wide range of applications [27], in particular also astrophysical applications [28].…”

Section: Ams Measurementsmentioning

confidence: 99%

AMS measurements of cosmogenic and supernova-ejected radionuclides in deep-sea sediment cores

Feige

Wallner

Fifield

et al. 2013

EPJ Web of Conferences

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Samples of two deep-sea sediment cores from the Indian Ocean are analyzed with accelerator mass spectrometry (AMS) to search for traces of recent supernova activity ∼2 Myr ago. Here, long-lived radionuclides, which are synthesized in massive stars and ejected in supernova explosions, namely 26 Al, 53 Mn and 60 Fe, are extracted from the sediment samples. The cosmogenic isotope 10 Be, which is mainly produced in the Earth's atmosphere, is analyzed for dating purposes of the marine sediment cores. The first AMS measurement results for 10 Be and 26 Al are presented, which represent for the first time a detailed study in the time period of 1.7-3.1 Myr with high time resolution. Our first results do not support a significant extraterrestrial signal of 26 Al above terrestrial background. However, there is evidence that, like 10 Be, 26 Al might be a valuable isotope for dating of deep-sea sediment cores for the past few million years.

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Applications of accelerator mass spectrometry

Cited by 94 publications

References 238 publications

The activation method for cross section measurements in nuclear astrophysics

The activation method for cross section measurements in nuclear astrophysics

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

AMS measurements of cosmogenic and supernova-ejected radionuclides in deep-sea sediment cores

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