Antiprotons in cosmic rays from neutralino annihilation
By F. Donato, N. Fornengo, D. Maurin, P. Salati, R. Torino, I. S. O. Physics, Kias SAp CEA-Saclay Lapth, Annecy. 2003
342 citations recorded by the source corpus.
We calculate the antiproton flux due to relic neutralino annihilations, in a two–dimensional diffusion model compatible with stable and radioactive cosmic ray nuclei. We find that the uncertainty in the primary flux induced by the propagation parameters alone is about two orders of magnitude at low energies, and it is mainly determined by the lack of knowledge on the thickness of the diffusive halo. On the contrary, different dark matter density profiles do not significantly alter the flux: a NFW distribution produces fluxes which are at most 20% higher than an isothermal sphere. The most conservative choice for propagation parameters and dark matter distribution normalization, together with current data on cosmic antiprotons, cannot lead to any definitive constraint on the supersymmetric parameter space, neither in a low–energy effective MSSM, or in a minimal SUGRA scheme. However, if the best choice for propagation parameters – corresponding to a diffusive halo of L = 4 kpc – is adopted, some supersymmetric configurations with the neutralino mass m� < 100 GeV should be considered as excluded. An enhancement flux factor - due for instance to a clumpy dark halo or to a higher local dark matter density - would imply a more severe cut on the supersymmetric parameters.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/1a8908421763821d2ce02c26c5fbe8c691a8290f
How researchers see this paper
The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.
In Astronomy and Astrophysics
In Nuclear and High Energy Physics
Citations in the corpus
- MadDM v.3.0: A comprehensive tool for dark matter studies (2018, neutral): “[47–51] and [26, 52–54] respectively.”
- Sneutrino cold dark matter, a new analysis: Relic abundance and detection rates (2007, methodology): “[77], where a detailed analysis which takes into account astrophysical uncertainties (relevant for the antiproton signal) are discussed.”
- Galactic secondary positron flux at the Earth (2008, background): “…uncertainties were calculated and quantified in Delahaye et al. (2008), where it was shown that they may be significant, especially in the low energy part of the spectrum, a property common also to the antiproton (e.g. Donato et al. 2004) and the antideuteron (Donato et al. 2000, 2008) signals.”
- Galactic electrons and positrons at the Earth: new estimate of the primary and secondary fluxes (2010, methodology): “…recall that almost all well-studied dark matter particle candidates, e.g. in the framework of supersymmetric or extra-dimensional theories, are expected to manifest themselves in neither the local positron nor antiproton spectra (e.g. Lavalle et al. 2008a; Delahaye et al. 2008; Donato et al. 2004).”
- Dark matter annihilations and decays after the AMS-02 positron measurements (2013, methodology): “[31] from an analysis of the primary antiproton flux from dark matter annihilations, and which is characterized by K0 = 0.”
- AMS-02 antiprotons, at last! Secondary astrophysical component and immediate implications for Dark Matter (2015, methodology): “Indeed, in this way the traditional Min-Med-Max schemes [31] are determined, and plausible ranges for the force field parameter of solar modulation (the so-called Fisk potential) are identified.”
- A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays - II. Results for the diffusion model combining B/C and radioactive nuclei (2010, methodology): “It has also been used to set constraints on dark matter annihilations in antinuclei (Donato et al. 2004), and positrons (Delahaye et al. 2008b).”