Cosmic ray antiprotons in the closed galaxy model

Protheroe, R. J.

doi:10.1086/159473

Cited by 64 publications

(25 citation statements)

References 11 publications

(18 reference statements)

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“…where for lower energies we have used the parametrization from Tan & Ng (1982), while in the high-energy range we apply the approximation given in Protheroe (1981). Both this parametrization and those needed above have been checked against a compilation of more recent data (Caso et al 1998).…”

Section: T Ertiary Antiprotonsmentioning

confidence: 99%

Cosmic Antiprotons as a Probe for Supersymmetric Dark Matter?

Bergström

Edsjö

Ullio

1999

ApJ

199

223

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The Ñux of cosmic-ray antiprotons from neutralino annihilations in the Galactic halo is computed for a large sample of models in the minimal supersymmetric extension of the standard model (MSSM). We also revisit the problem of estimating the background of low-energy cosmic-rayÈinduced secondary antiprotons, taking into account their subsequent interactions (and energy loss) and the presence of nuclei in the interstellar matter. We consider a two-zone di †usion model, with and without a Galactic wind. We Ðnd that, given the uncertainties in the background predictions, there is no need for a primary (exotic) component to explain current data. However, allowing for a signal by playing with the uncertainties in the background estimate, we discuss the characteristic features of the supersymmetric models that give a satisfactory description of the data. We point out that in some cases, the optimal kinetic energy to search for a signal from supersymmetric dark matter is above several GeV, rather than the traditional sub-GeV region. The large astrophysical uncertainties involved do not, on the other hand, allow the exclusion of any of the MSSM models we consider on the basis of data. In addition to numerical results, we also present convenient parameterizations of the antiproton yields of all "" basic ÏÏ two-body Ðnal states. We also give examples of the yield and di †erential energy spectrum for a set of supersymmetric models with high rates. We also remark that it is difficult to set a limit on the antiproton lifetime from present measurements, since the injection of antiprotons from neutralino annihilation can compensate for the loss from decay.

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Section: T Ertiary Antiprotonsmentioning

confidence: 99%

Cosmic Antiprotons as a Probe for Supersymmetric Dark Matter?

Bergström

Edsjö

Ullio

1999

ApJ

199

223

View full text Add to dashboard Cite

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“…Fig.5 shows how sensitively, at fixed m χ , this ratio depends on the neutralino composition. In this figure also the background due to the secondary antiprotons produced in cosmic-ray collisions in the interstellar medium is displayed [29].…”

Section: Results and Conclusionmentioning

confidence: 99%

“…Figure 5 Antiproton-to-proton flux ratio,p/p, as a function of the kinetic energy T , for m χ = 30 GeV and for different neutralino compositions: P = 10 −3 (long-short dashed curve); P = 0.1 (solid curve); P = 0.5 (long dashed curve); P = 0.9 (dash-dotted curve); P = 0.999 (short dashed curve). The dotted curve is the background flux of secondary antiprotons, calculated in the leaky-box model [29]. Here tan β = 8, m h = 50 GeV and mf = 45GeV.…”

Section: Results and Conclusionmentioning

confidence: 99%

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Amount of antiprotons in cosmic rays due to halo neutralino annihilation

Bottino

Favero

Fornengo

et al. 1995

Astroparticle Physics

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We evaluate the antiproton-to-proton flux ratio which can be generated by neutralino-neutralino annihilation in the galactic halo, considering the most general compositions for the relic neutralinos and modelling the neutralino local density according to its relic abundance. We find that in the case of mixed neutralino compositions this p/p ratio is higher than for pure higgsinos or gauginos. It is shown how the expected improvements in sensitivity for the new measurements of thep/p may provide very useful information, complementary to the one obtainable with other experimental means.( to appear in Astroparticle Physics )

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“…[14]) and inelastic collisions (see [15] for details). The source term of antiprotons incoming from outside the Galaxy, Q(E) in Eq.…”

Section: Models Of Secondary Antiproton Productionmentioning

confidence: 99%

Modulated antiproton fluxes for interstellar production models

Boella

Gervasi

Potenza

et al. 1998

Astroparticle Physics

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Expected differential fluxes of antiprotons at the Earth's orbit are calculated for minimum and medium strength of the solar modulation. We used an analytical solution in the force-field approximation. Local interstellar spectra are taken as predictions of different theoretical models of secondary production of antiprotons in the Galaxy. All the antiproton-as well as proton-fluxes are modulated in the same way for the purpose of a direct comparison in order to avoid additional uncertainties. It is shown that, in order to compare experimental data with the existing models predictions, next generation experiments should be able to measure fluxes of particles with energies above 100 MeV. c 1998 Elsevier Science B.V.

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Cosmic ray antiprotons in the closed galaxy model

Cited by 64 publications

References 11 publications

Cosmic Antiprotons as a Probe for Supersymmetric Dark Matter?

Cosmic Antiprotons as a Probe for Supersymmetric Dark Matter?

Amount of antiprotons in cosmic rays due to halo neutralino annihilation

Modulated antiproton fluxes for interstellar production models

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