An anomalous positron abundance in cosmic rays with energies 1.5–100 GeV

By O. Adriani, G. Barbarino, Galina Bazilevskaya, R. Bellotti, M. Boezio, É. Bogomolov, L. Bonechi, M. Bongi, V. Bonvicini, S. Bottai and 41 more. Nature, 2009

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Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a6dd395f9a014add64e2905e3dd1e2cc85e3b2a3

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Citations in the corpus

AMS-02 antiprotons, at last! Secondary astrophysical component and immediate implications for Dark Matter (2015, background): “The spectra are measured up to a rigidity of 1.8 and 3 TV for p and α nuclei, respectively, and, as already reported by the Pamela Collaboration [29], they cannot be described by a single power law: a hardening at energies higher than ∼300 GV is observed for both.”
Dark matter direct-detection experiments (2015, background): “Finally, also charged particles like protons, antiprotons, electrons and positrons can be detected by satellites. Measurements on the steadily increasing positron fraction from 10 to ˘250GeV by Pamela[94] and AMS[95] rise discussions on its possible dark matter origin. However, given that such a spe”
A database of charged cosmic rays (2013, neutral): “…– OGO5 (1968/06-1968/10): Fulks (1975) – OGO5 (1969/06-1969/07): Fulks (1975); Burger & Swanenburg (1974) – OGO5 (1970/06-1970/07): Fulks (1975); Burger & Swanenburg (1974) – OGO5 (1971/05-1971/08): Fulks (1975) – OGO5 (1971/07-1971/08): Burger & Swanenburg (1974) – OGO5 (1972/06): Fulks (1975) –…”
The Phenomenology of Right Handed Neutrinos (2013, background): “straints, 5Others include the long standing issues of the muon magnetic moment (see e.g. [3] for a review), the annual modulation in the DAMA data [4], the excess of positrons in the cosmic radiation [5, 6], the ”forward-backward asymmetry” observed at the Tevatron [7], the disputed evidence for neu”
THE PHYSICS OF THE FAR-INFRARED–RADIO CORRELATION. I. CALORIMETRY, CONSPIRACY, AND IMPLICATIONS (2009, background): “Above ∼ 1 GeV, the observed positron flux exceeds the predicted flux even in detailed models (see Moskalenko & Strong 1998; Beatty et al. 2004; Adriani et al. 2009; but see Delahaye et al. 2009).”
Particle acceleration in axisymmetric pulsar current sheets (2014, positive): “In another publication, we will explore if this result can be related to the contribution of pulsars to the rising positron fraction measured by PAMELA (Adriani et al. 2009).”
TIME DEPENDENCE OF THE e− FLUX MEASURED BY PAMELA DURING THE 2006 JULY–2009 DECEMBER SOLAR MINIMUM (2013, background): “PAMELA has provided important results on the antiproton (Adriani et al. 2009a) and positron (Adriani et al. 2009b) galactic abundances.”
Abelian hidden sectors at a GeV (2009, methodology): “The PAMELA [18], ATIC [19], and PPB-BETS [20] experiments observe excesses in cosmic ray positrons and electrons at energies above 10 GeV.”