Importance of nuclear physics to NASA’s space missions

Tripathi, R. K.; Wilson, John W.; Cucinotta, Francis A.

doi:10.1063/1.1469938

Cited by 9 publications

(26 citation statements)

References 2 publications

(2 reference statements)

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“…the covariance matrix is sensitive to the choice of propagation parameters. Since we want to avoid evaluating (32) for each set of propagation parameters, we define the relative covariance matrix…”

Section: Discussionmentioning

confidence: 99%

“…Annihilation in the galactic disc on the other hand is mainly relevant for hadronic cosmic rays. The annihilation cross sections for nuclei are taken from [31,32] and for antiprotons from [33,34]. 2 In the case of antiprotons we also have to consider inelastic (non-annihilating) scattering with the interstellar matter.…”

Section: Diffusion Modelmentioning

confidence: 99%

“…The latter is obtained in complete analogy to Σ B/C,source by mapping uncertainties in cross section and primary flux parameters into uncertainties in the antiproton flux (see appendix A). The full covariance matrix Σ p includes the experimental errors of AMS-02 and enters the χ 2 -test as in (31). We account for solar modulation via the Fisk potential φ − AMS-02 defined in (11).…”

Section: Antiproton and B/c Fitmentioning

confidence: 99%

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A precision search for WIMPs with charged cosmic rays

Reinert¹,

Winkler²

2018

J. Cosmol. Astropart. Phys.

156

214

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AMS-02 has reached the sensitivity to probe canonical thermal WIMPs by their annihilation into antiprotons. Due to the high precision of the data, uncertainties in the astrophysical background have become the most limiting factor for indirect dark matter detection. In this work we systematically quantify and -where possible -reduce uncertainties in the antiproton background. We constrain the propagation of charged cosmic rays through the combination of antiproton, B/C and positron data. Cross section uncertainties are determined from a wide collection of accelerator data and are -for the first time ever -fully taken into account. This allows us to robustly constrain even subdominant dark matter signals through their spectral properties. For a standard NFW dark matter profile we are able to exclude thermal WIMPs with masses up to 570 GeV which annihilate into bottom quarks. While we confirm a reported excess compatible with dark matter of mass around 80 GeV, its local (global) significance only reaches 2.2 σ (1.1 σ) in our analysis.

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Section: Discussionmentioning

confidence: 99%

Section: Diffusion Modelmentioning

confidence: 99%

Section: Antiproton and B/c Fitmentioning

confidence: 99%

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A precision search for WIMPs with charged cosmic rays

Reinert¹,

Winkler²

2018

J. Cosmol. Astropart. Phys.

156

214

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“…For 'ion physics' of alpha-particles, protons, and H isotope nuclei we used the cross section by Tripathi et al [14], holding for energies of up to 20 GeV per nucleon. The cross sections used for the other ions [15] are valid only up to 10 GeV per nucleon.…”

Section: Appendix B: the Physics Modelmentioning

confidence: 99%

Simulations of galactic cosmic ray impacts on the Herschel/PACS bolometer arrays with Geant4 code

et al. 2008

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The effects of the in-flight behaviour of the bolometer arrays of the Herschel/Photo-conductor Array Camera and Spectrometer (PACS) instrument under impacts of Galactic cosmic rays are explored. This instrument is part of the ESA-Herschel payload, which will be launched at the end of 2008 and will operate at the Lagrangian L2 point of the Sun-Earth system. We find that the components external to the detectors (the spacecraft, the cryostat, the PACS box, collectively referred to as the 'shield') are the major source of secondary events affecting the detector behaviour. The impacts deposit energy on the bolometer chips and influence the behaviour of nearby pixels. 25% of hits affect the adjacent pixels. The energy deposited raises the bolometer temperature by a factor ranging from 1 to 6 percent of the nominal value. We discuss the effects on the observations and compare simulations with laboratory tests

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“…Five methods/models are used in the Geant4 toolkit [1] for calculations of nucleus-nucleus cross sections: LHEP originated from Geant3, Kox [2], Sihver [3], Shen [4] and Tripathi [5,6]. They are implemented in the corresponding classes: G4HadronCrossSections, G4IonsKoxCrossSection, G4IonsSihver CrossSection, G4IonsShenCrossSection, G4TripathiCrossSection, G4TripathiLightCrossSection.…”

mentioning

confidence: 99%

Calculation of light nucleus reaction cross sections in Geant4

Uzhinsky

2012

Preprint

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Total reaction cross sections of light projectile nucleus ( 2 H, 3 H, 3 He and 4 He) interactions with nuclei are calculated using Geant4 models, and compared with experimental data. It is shown that the models give various predictions at low energies, in the region of the Coulomb barrier. "Shen model" (W.-Q. Shen et al., Nucl. Phys. A491 (1989) 130) is identified as an improvement over other models.

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Importance of nuclear physics to NASA’s space missions

Cited by 9 publications

References 2 publications

A precision search for WIMPs with charged cosmic rays

A precision search for WIMPs with charged cosmic rays

Simulations of galactic cosmic ray impacts on the Herschel/PACS bolometer arrays with Geant4 code

Calculation of light nucleus reaction cross sections in Geant4

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