Helium in near Earth orbit

By J. Alcaraz, B. Alpat, G. Ambrosi, H. Anderhub, L. Ao, A. Arefiev, P. Azzarello, E. Babucci, L. Baldini, M. Basile and 190 more. 2000

150 citations recorded by the source corpus.

Abstract The helium spectrum from 0.1 to 100 GeV/nucleon was measured by the Alpha Magnetic Spectrometer (AMS) during space shuttle flight STS-91 at altitudes near 380 km. Above the geomagnetic cutoff the spectrum is parameterized by a power law. Below the geomagnetic cutoff a second helium spectrum was observed. In the second helium spectra over the energy range 0.1 to 1.2 GeV/nucleon the flux was measured to be (6.3±0.9)×10 −3 ( m 2 sec sr ) −1 and more than ninety percent of the helium was determined to be 3 He (at the 90% CL). Tracing helium from the second spectrum shows that about half of the 3 He travel for an extended period of time in the geomagnetic field and that they originate from restricted geographic regions similar to protons and positrons.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/52e71f0ac8fd2417d2b26661b174789c013b1f32

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In Astronomy and Astrophysics

1. I. Usoskin
2. G. Kovaltsov
3. A. Mishev
4. D. Maurin
5. R. Taillet
6. P. Salati
7. E. Seo
8. Aurélien Barrau

In Molecular Biology

1. I. Usoskin
2. G. Kovaltsov
3. A. Mishev
4. F. Joos
5. R. Roth
6. S. Solanki
7. Paul Charbonneau
8. N. Krivova

Citations in the corpus

• Antiprotons from Spallations of Cosmic Rays on Interstellar Matter (2001, methodology): “Recent measurements made by the balloon-borne spectrometer BESS (Sanuki et al. 2000) and by the AMS detector during the space shuttle Ñight (Alcaraz et al. 2000a, 2000b, 2000c) dramatically reduced the uncertainties both on proton and helium spectra.”
• A new model of cosmogenic production of radiocarbon 14C in the atmosphere (2012, background): “…(in particle number) to LIS of GCR leading to the nucleonic fraction of heavier species to protons of the160 order of 0.25-0.3 outside the heliosphere (e.g. Alcaraz et al., 2000a,b; Adriani et al., 2011; Webber and Higbie, 2003;161 Nakamura et al., 2010), viz. half of that assumed by MB09.”
• A database of charged cosmic rays (2013, unknown): “…& Evenson (2002) – AESOP00 (2000/08): Clem & Evenson (2002) – AESOP02 (2002/08): Clem & Evenson (2004) – AESOP06 (2006/08): Clem & Evenson (2009) – ALICE – ALICE (1987/08): Hesse et al. (1996) – ALICE (1987/08+1987/08): Esposito et al. (1992) – AMS-01 – AMS01 (1998/06): Alcaraz et al. (2000a);…”
• DISCREPANT HARDENING OBSERVED IN COSMIC-RAY ELEMENTAL SPECTRA (2010, methodology): “The CREAM elemental fluxes are compared with selected previous data (Asakimori et al. 1998; Derbina et al. 2005; Zei et al. 2007; Ahn et al. 2007b; Alcaraz et al. 2000; Panov et al. 2009): CREAM-1 (filled circles), CREAM-2 (filled squares), AMS (stars), BESS (open squares), JACEE (X), RUNJOB…”