Measurements of 0.2–20 GeV/n cosmic-ray proton and helium spectra from 1997 through 2002 with the BESS spectrometer

By Y. Shikaze, S. Haino, K. Abe, H. Fuke, T. Hams, K. C. Kim, Y. Makida, S. Matsuda, J. Mitchell, A. Moiseev and 14 more. 2006

192 citations recorded by the source corpus.

Abstract We measured low energy cosmic-ray proton and helium spectra in the kinetic energy range 0.215–21.5 GeV/n at different solar activities during a period from 1997 to 2002. The observations were carried out with the BESS spectrometer launched on a balloon at Lynn Lake, Canada. A calculation for the correction of secondary particle backgrounds from the overlying atmosphere was improved by using the measured spectra at small atmospheric depths ranging from 5 through 37 g/cm 2 . The uncertainties including statistical and systematic errors of the obtained spectra at the top of atmosphere are 5–7% for protons and 6–9% for helium nuclei in the energy range 0.5–5 GeV/n.

Subfields: Nuclear and High Energy Physics, Pulmonary and Respiratory Medicine

View Paper: https://www.semanticscholar.org/paper/59cad9b073d1ad7225850e5451b5c2ba0e565cca

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Nuclear and High Energy Physics

In Pulmonary and Respiratory Medicine

F. Ryde

Citations in the corpus

DEVELOPMENT OF THE MODEL OF GALACTIC INTERSTELLAR EMISSION FOR STANDARD POINT-SOURCE ANALYSIS OF FERMI LARGE AREA TELESCOPE DATA (2016, methodology): “…30 GeV using the γ-ray production cross-section of Kamae et al. (2006) and a CR proton flux spectrum parametrized as: bA RP P1 2, where b = v c is the proton-to-light velocity ratio, R is the proton rigidity, A is a free normalization, and P1 and P2 are free spectral indices (Shikaze et al. 2007).”
FERMI OBSERVATIONS OF CASSIOPEIA AND CEPHEUS: DIFFUSE GAMMA-RAY EMISSION IN THE OUTER GALAXY (2009, background): “The proton spectrum is derived from a compilation of direct measurements (Alcaraz et al. 2000; Sanuki et al. 2000; Shikaze et al. 2007).”
Dark Matter Searches with Astroparticle Data (2011, background): “…such as NASA’s Advanced Composition Explorer (ACE; Stone et al., 1998), to orbiting particle detectors such as PAMELA (Picozza et al., 2007), to massive balloon payloads, e.g., BESS (Shikaze et al., 2007), to enormous ground-based arrays such as the Pierre Auger Observatory (Abraham et al., 2004).”
RECORD-SETTING COSMIC-RAY INTENSITIES IN 2009 AND 2010 (2010, background): “During 1997–2008 there is an excellent correlation between the E9 count rate and >120 MeV proton intensities from the BESS balloon-borne instrument (Shikaze et al. 2007) and PAMELA mission (Casolino et al. 2009), relating the E9 count rate and >120 MeV proton intensity with ∼2% accuracy.”
Galactic electrons and positrons at the Earth: new estimate of the primary and secondary fluxes (2010, background): “Fits of the proton and α particle fluxes are provided in Shikaze et al. (2007), based on various measurements at the Earth.”
A database of charged cosmic rays (2013, unknown): “…Wang et al. (2002) – BESS94 (1994/07): Myers et al. (2003) – BESS95 (1995/07): Matsunaga et al. (1998); Myers et al. (2003) – BESS97 (1997/07): Orito et al. (2000); Myers et al. (2003); Shikaze et al. (2007) – BESS98 (1998/07): Sanuki et al. (2000); Maeno et al. (2001); Myers et al.…”
Galactic secondary positron flux at the Earth (2008, methodology): “In this analysis, we adopt the determinations of Shikaze et al. (2007) and Donato et al. (2001).”