Peter BIERMANN (.pdf)

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detection of a 130 GeV emission line, vii) an upturn in the CR-spectra of all elements from Helium, with a hint of an upturn for Hydrogen, viii) a derivation of the interaction grammages separately for CR-protons and CR-heavy nuclei, and ix) the complete cosmic ray spectrum with a steep powerlaw leading to a dip near 3 1018 eV in terms of E3 (dN/dE), then a broad bump near 5 1019 eV, turning down towards 1021 eV (KASCADE, IceTop, KASCADE- Grande, Auger). All these features can be quantitatively explained, eliminating any argument from supersymmetry. These explanations build on the action of cosmic rays accelerated in the magnetic winds of very massive stars, when they explode (Biermann et al. 2009 - 2012): this work is based on predictions from 1993 (Biermann 1993, Biermann & Cassinelli 1993, Biermann & Strom 1993, Stanev et al 1993; review at ICRC Calgary 1993); this approach is older and simpler than adding WR-star su- 30
pernova CR-contributions with pulsar wind nebula CRcontributions, is also simpler than using magnetic field enhancement in ISM-shocks, and also simpler than using the decay of a postulated particle; this approach also gave quantitative predictions from 1993 which can now be tested. This concept gives an explanation for the cosmic ray spectrum as Galactic plus one extragalactic source, Cen A (Gopal-Krishna et al. 2010, Biermann & de Souza 2012). The data do not require any extra source population below the MWBG induced turnoff - commonly referred to as the GZK-limit: Greisen (1966), Zatsepin & Kuzmin (1966); in fact the cut-off observed in the spectrum may well derive from an energy limit in the source due to spatial limits. All this is possible, since the magnetic horizon appears to be quite small (consistent with the cosmological MHD simulations of Ryu et al. 2008). It also entails that Cen A is our highest energy physics lab- 31
Page 1 and 2: ASTROPHYSICS OF WARM DARK MATTER Pe
Page 3 and 4: AMS positron fraction: data 2013 3
Page 5 and 6: CR positron fraction: prediction 20
Page 7 and 8: Supersymmetry! Evidence? • Supers
Page 9 and 10: Cosmic ray knee: paper CR-IV, 1993
Page 11 and 12: 130 GeV line interpreted ? • Rece
Page 13 and 14: Summary cosmic ray particles • Qu
Page 15 and 16: The sky in black holes > ∼108 M
Page 17 and 18: Massive and supermassive stars at v
Page 19 and 20: Stellar agglomeration conditions
Page 21 and 22: The radio background, Thomson depth
Page 23 and 24: The radio background, Thomson depth
Page 25 and 26: Energy density from ∼ 3 106 M⊙
Page 27 and 28: ? ? Weakly Interacting Neutrino = W
Page 29: 2 Abstract Dark matter has been fir
Page 33 and 34: massive black holes: they possibly
Page 35 and 36: HII regions and HNRs, and only a ve
Page 37 and 38: [11] Adulpravitchai, A., Gu, P.-H.,
Page 39 and 40: [19] Bringmann, T., et al., eprint
Page 41 and 42: Strom, Astron. & Astroph. 275, 659
Page 43 and 44: [34] Universality of galactic surfa

Peter BIERMANN (.pdf)

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