COSMIC-RAY PROTON AND HELIUM SPECTRA FROM THE FIRST CREAM FLIGHT

By Y. Yoon, H. Ahn, P. Allison, M. G. Bagliesi, J. Beatty, G. Bigongiari, P. Boyle, J. Childers, N. Conklin, S. Coutu and 24 more. 2011

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Cosmic-ray proton and helium spectra have been measured with the balloon-borne Cosmic Ray Energetics And Mass experiment flown for 42 days in Antarctica in the 2004–2005 austral summer season. High-energy cosmic-ray data were collected at an average altitude of ∼38.5 km with an average atmospheric overburden of ∼3.9 g cm−2. Individual elements are clearly separated with a charge resolution of ∼0.15 e (in charge units) and ∼0.2 e for protons and helium nuclei, respectively. The measured spectra at the top of the atmosphere are represented by power laws with a spectral index of −2.66 ± 0.02 for protons from 2.5 TeV to 250 TeV and −2.58 ± 0.02 for helium nuclei from 630 GeV nucleon−1 to 63 TeV nucleon−1. They are harder than previous measurements at a few tens of GeV nucleon−1. The helium flux is higher than that expected from the extrapolation of the power law fitted to the lower-energy data. The relative abundance of protons to helium nuclei is 9.1 ± 0.5 for the range from 2.5 TeV nucleon−1 to 63 TeV nucleon−1. This ratio is considerably smaller than the previous measurements at a few tens of GeV nucleon−1.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8506dd079d6ee7fe3909664e8ec7bb7214467731

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In Astronomy and Astrophysics

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In Nuclear and High Energy Physics

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Citations in the corpus

• Proton and Helium Spectra from the CREAM-III Flight (2017, background): “Elemental spectra from the first two CREAM flights were reported in Ahn et al. (2007, 2009, 2010) and Yoon et al. (2011) [2, 3, 4, 5].”
• Cosmic-ray energy spectrum and composition up to the ankle - the case for a second Galactic component (2016, background): “…nuclei with respect to the proton spectrum (Adriani et al. 2011), and the spectral hardening of both the proton and helium nuclei at TeV energies (Yoon et al. 2011), are di cult to explain using standard models of cosmic-ray acceleration in supernova remnants and their subsequent propagation in…”
• Cosmic ray transport in the Galaxy: A review (2017, methodology): “The data points are the measurements by Voyager (empty circles, Stone et al. (2013)), AMS-02 (filled circles, Aguilar et al. (2015b)), PAMELA (empty squares, Adriani et al. (2011b)), and CREAM (filled squares, Yoon et al. (2011)).”
• A database of charged cosmic rays (2013, unknown): “…(2004/01): Yoshida et al. (2008) – CAPRICE – CAPRICE94 (1994/08): Boezio et al. (1997, 1999, 2000) A32, page 10 of 13 – CAPRICE98 (1998/05): Boezio et al. (2001a,b); Mocchiutti & Wizard/Caprice Collaboration (2003); Boezio et al. (2003); Papini et al. (2004) – CREAM – CREAM-I…”
• DEVELOPMENT OF THE MODEL OF GALACTIC INTERSTELLAR EMISSION FOR STANDARD POINT-SOURCE ANALYSIS OF FERMI LARGE AREA TELESCOPE DATA (2016, methodology): “Near Earth, the compilation of PAMELA (Adriani et al. 2011), AMS-02 (Aguilar et al. 2015), CREAM (Yoon et al. 2011), and ATIC-2 (Panov et al. 2006) data indicates an up-turn in the proton spectrum starting around 500GV.”