The Absolute Flux of Protons and Helium at the Top of the Atmosphere Using IMAX

By W. Menn, M. Hof, O. Reimer, M. Simon, A. Davis, A. Labrador, R. Mewaldt, S. M. Schindler, L. Barbier, E. Christian and 9 more. 2000

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THE PHYSICS OF THE FAR-INFRARED–RADIO CORRELATION. I. CALORIMETRY, CONSPIRACY, AND IMPLICATIONS (2009, unknown): “…energies (γ ≫ 1), the observed CR electrons have (e.g., Longair 1994) dIe dE = cNe(E) 4π = 0.07 ( E GeV )−3.3 cm−2 s−1 sr−1 GeV−1 (15) 7 and the observed CR protons have (e.g., Mori 1997; Menn et al. 2000; AMS Collaboration et al. 2002) dIp dE = cNp(E) 4π ≈ 1.5 ( E GeV )−2.7 cm−2 s−1 sr−1 GeV−1.”
The Cosmic-Ray Antiproton Flux between 3 and 49 GeV (2001, background): “To construct this distribution events that suffered multiple Coulomb scattering had to be eliminated since they could enlarge the distribution (see Menn et al. 2000).”
Badhwar–O’Neill galactic cosmic ray model update based on advanced composition explorer (ACE) energy spectra from 1997 to present (2004, methodology): “IMAX (Menn et al., 2000), launched in Canada in 1992 with a geometric factor of 142 cm-sr measured proton and helium spectra in a 16 hour flight - but no heavy ion spectra.”
A database of charged cosmic rays (2013, unknown): “…Barwick et al. (1995, 1997, 1998) – HEAT95 (1995/08): Barwick et al. (1997); DuVernois et al. (2001) – HEAT94&95 (1994/05+1995/08): Barwick et al. (1997); DuVernois et al. (2001) – HEAT-pbar (2000/06): Beach et al. (2001); Beatty et al. (2004) – HEIST (1988/08): Gibner et al. (1992) – IMAX92…”