Tran - DESY Theory workshop 2008

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The Antiproton Spectrum Similar propagation mechanism as in the case of positrons We neglect effects of reacceleration and tertiary contributions Huge uncertainties due to degeneracies in the determination of the propagation parameters Primary antiproton flux can vary by two orders of magnitude for parameters compatible with the Boron-to-Carbon ratio David Tran Indirect Signatures of Gravitino Dark Matter with Broken R-Parity
The Antiproton Spectrum Primary top-of-atmosphere antiproton spectrum: 10 1 0.1 1 10 100 Antiproton flux [GeV -1 m -2 s -1 sr -1 ] 10 0 10 -1 10 -2 10 -3 MAX MED MIN BESS 95+97 BESS 95 IMAX 92 CAPRICE 94 CAPRICE 98 Φ = 500 MV 10 -4 [A. Ibarra, DT 2008] T [GeV] m 3/2 = 150 GeV, τ 3/2 = 1.3 × 10 26 s, different sets of propagation parameters. Dangerous overproduction of antiprotons → for MED, MAX parameters, the model is probably not phenomenologically viable David Tran Indirect Signatures of Gravitino Dark Matter with Broken R-Parity
Page 1 and 2: Indirect Signatures of Gravitino Da
Page 3 and 4: Outline Based on A. Ibarra and D. T
Page 5 and 6: Indirect Detection Even for graviti
Page 7 and 8: The Gamma-Ray Spectrum The diffuse
Page 9 and 10: The Gamma-Ray Spectrum Calculate de
Page 11 and 12: The Gamma-Ray Spectrum Spectrum for
Page 13 and 14: The Gamma-Ray Spectrum Heavier grav
Page 15 and 16: The Gamma-Ray Spectrum Fragmentatio
Page 23 and 24: Outline 1 Gravitino Dark Matter 2 G
Page 25 and 26: The Positron Fraction Propagation i
Page 27 and 28: The Positron Fraction Experiments u
Page 29 and 30: The Positron Fraction Using the EGR
Page 31 and 32: The Positron Fraction The coinciden
Page 33: The Antiproton Spectrum Theoretical
Page 41 and 42: Overview of the Indirect Signatures

Tran - DESY Theory workshop 2008

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