Peter BIERMANN (.pdf)

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Planck, WMAP, Fermi haze/bubble, 511 keV • Polar cap CR-electron component: with diffusion E−7/3 , radio spectrum ν−2/3 • In GC region transition between diffusion dominance and loss dominance shifted to higher particle energy – smaller scale height: Reproduces flux, radial profile • Spectrum predicted: ν−2/3 , ν−1 , ν−3/2 : confirmed by Fermi haze (2010), consistent with Planck haze (2012), the IC component: flat in E2 γ F (Eγ) 10 • Fermi bubble: unstable galactic magnetic wind driven by CRs from non-steady star-formation? • Correct number of positrons for 511 keV emission: grammage for ISM-SN-CRs about 1 gm/cm2 , and for wind- SN-CRs about 10 gm/cm2 (Nath et al. MN Lett 2012) • PLB et al., ApJL 710, L53 (2010): Planck haze data!
130 GeV line interpreted ? • Recent claims that 130 GeV emission line in Galactic Center region, Su & Finkbeiner 1206.1616; Buckley & Hooper 1205.6811; Weniger 1204.2797; Bringmann et al. 1203.1312. • Decay of dark matter particle? • Work with Nayantara Gupta and Biman Nath (RRI, Bangalore) 11 • Consider CR-electron spectrum, flat in E 3 J(E) • Consider radiation field, Moskalenko et al. 2006, peaks at 1 µ and at 100 µ • Inverse Compton by these CR-electrons gives equivalent contributions, fully explaining the weak line: pair production gives narrow feature in IC! • Confirms that CR-electron spectra similar in GC region
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: Cosmic ray knee: paper CR-IV, 1993
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 and 30: 2 Abstract Dark matter has been fir
Page 31 and 32: pernova CR-contributions with pulsa
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

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