Cosmic-Ray Electrons and Positrons from 1 to 100 GeV: Measurements with HEAT and Their Interpretation

By M. DuVernois, S. Barwick, J. Beatty, A. Bhattacharyya, C. Bower, C. Chaput, S. Coutu, G. Nolfo, D. Lowder, S. McKee and 8 more. 2001

201 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/44095bfe06fb21b40be17f6039fe5c909b2fe1d1

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In Astronomy and Astrophysics

1. E. Orlando
2. A. Strong
3. T. Jaffe
4. N. Fornengo
5. R. Lineros
6. J. Lavalle
7. T. Delahaye
8. A. Ibarra

In Nuclear and High Energy Physics

1. E. Orlando
2. A. Strong
3. N. Fornengo
4. T. Jaffe
5. R. Lineros
6. J. Lavalle
7. T. Delahaye
8. A. Ibarra

Citations in the corpus

• A database of charged cosmic rays (2013, unknown): “…Ackermann et al. (2010) – H.E.S.S. (2004/10-2007/08): Aharonian et al. (2008, 2009) – HEAO3-C2 (1979/10-1980/06): Ferrando et al. (1988); Engelmann et al. (1990) – HEAT – HEAT94 (1994/05): Barwick et al. (1995, 1997, 1998) – HEAT95 (1995/08): Barwick et al. (1997); DuVernois et al. (2001) –…”
• The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements. (2011, methodology): “The CR electron and positron data used are as follows: AMS01 (AMS Collaboration et al. 2002), CAPRICE94 (Boezio et al. 2000), HEAT (DuVernois et al. 2001), SANRIKU (Kobayashi 1999), BETS (Torii et al. 2001), PPT-BETS (Yoshida et al. 2008), ATIC-1-2 (Chang et al. 2008), H.E.S.S. (Aharonian et al.…”
• Dark matter annihilations and decays after the AMS-02 positron measurements (2013, methodology): “tter annihilations (left plot) and dark matter decays (right plot). Lastly, we compare in Fig. 5 the limits on the annihilation cross section or lifetime derived from the positron ux measured by HEAT [2], PAMELA [5] and AMS-02 [7], as well as from the positron fraction measured by AMS-02 [6], assumi”
• Parameterization of γ, epm, and Neutrino Spectra Produced by p-p Interaction in Astronomical Environments (2006, unknown): “We note that space-borne experiments such as PAMELA3 will soon measure the electron and positron spectra in the sub-TeV energy range, where the secondaries of p−p interaction may become comparable to the primary components (Müller 2001; Stephens 2001; DuVernois et al. 2001).”
• Galactic electrons and positrons at the Earth: new estimate of the primary and secondary fluxes (2010, methodology): “We therefore only use the electron data from CAPRICE (Boezio et al. 2000), HEAT (DuVernois et al. 2001), and AMS-01 (Alcaraz et al. 2000), to avoid any confused interpretation mixing positrons.”