Antiprotons in cosmic rays from neutralino annihilation

Donato, Fiorenza; Fornengo, N.; Maurin, D.; Salati, Pierre; Taillet, R.

doi:10.1103/physrevd.69.063501

Cited by 362 publications

(627 citation statements)

References 65 publications

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“…As antimatter seems to be scarce in the Universe, apparently with no standard primary sources, there is a chance that by measuring antimatter in cosmic ray fluxes one may find evidence of the existence of dark matter particles (see, e.g., [91,92,93,94,95,96,97,98,99]). In the current release of the code we consider neutralino induced fluxes of antiprotons, positrons and antideuterons.…”

Section: Indirect Searches Through Antimatter Signalsmentioning

confidence: 99%

DarkSUSY: computing supersymmetric dark matter properties numerically

Gondolo

Edsjö

Ullio

et al. 2004

J. Cosmol. Astropart. Phys.

909

1,059

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The question of the nature of the dark matter in the Universe remains one of the most outstanding unsolved problems in basic science. One of the best motivated particle physics candidates is the lightest supersymmetric particle, assumed to be the lightest neutralino -a linear combination of the supersymmetric partners of the photon, the Z boson and neutral scalar Higgs particles. Here we describe DarkSUSY, a publicly-available advanced numerical package for neutralino dark matter calculations. In DarkSUSY one can compute the neutralino density in the Universe today using precision methods which include resonances, pair production thresholds and coannihilations. Masses and mixings of supersymmetric particles can be computed within DarkSUSY or with the help of external programs such as FeynHiggs, ISASUGRA and SUSPECT. Accelerator bounds can be checked to identify viable dark matter candidates. DarkSUSY also computes a large variety of astrophysical signals from neutralino dark matter, such as direct detection in low-background counting experiments and indirect detection through antiprotons, antideuterons, gamma-rays and positrons from the Galactic halo or high-energy neutrinos from the center of the Earth or of the Sun. Here we describe the physics behind the package. A detailed manual will be provided with the computer package.

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Section: Indirect Searches Through Antimatter Signalsmentioning

confidence: 99%

DarkSUSY: computing supersymmetric dark matter properties numerically

Gondolo

Edsjö

Ullio

et al. 2004

J. Cosmol. Astropart. Phys.

909

1,059

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“…Typical combinations of diffusion parameters that are compatible with the B/C analysis . As shown in Donato et al (2004), these propagation models correspond respectively to minimal, medium, and maximal primary antiproton fluxes.…”

Section: Propagation Parametersmentioning

confidence: 99%

“…3.3 for additional details). This model has been consistently used in several studies to constrain the propagation parameters Donato et al 2002) and examine their consequences for the standard p flux , the exotic p and d fluxes (Maurin et al , 2006Donato et al 2004;Barrau et al 2002Barrau et al , 2005Bringmann & Salati 2007), and also for positrons (Lavalle et al 2008b;Delahaye et al 2008). The reader is referred to Maurin et al (2001) for a more detailed presentation and motivation of the framework.…”

Section: Propagationmentioning

confidence: 99%

“…The related astrophysical 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 signals. For positrons, sizeable fluxes from dark matter annihilation are typically possible if dark matter overdensities are locally present, which is usually coded into the socalled "boost factor".…”

Section: Introductionmentioning

confidence: 99%

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Galactic secondary positron flux at the Earth

Delahaye

Lineros²,

Donato³

et al. 2009

A&A

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217

308

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Context. Secondary positrons are produced by spallation of cosmic rays within the interstellar gas. Measurements have been typically expressed in terms of the positron fraction, which exhibits an increase above 10 GeV. Many scenarios have been proposed to explain this feature, among them some additional primary positrons originating from dark matter annihilation in the Galaxy. Aims. The PAMELA satellite has provided high quality data that has enabled high accuracy statistical analyses to be made, showing that the increase in the positron fraction extends up to about 100 GeV. It is therefore of paramount importance to constrain theoretically the expected secondary positron flux to interpret the observations in an accurate way. Methods. We focus on calculating the secondary positron flux by using and comparing different up-to-date nuclear cross-sections and by considering an independent model of cosmic ray propagation. We carefully study the origins of the theoretical uncertainties in the positron flux. Results. We find the secondary positron flux to be reproduced well by the available observations, and to have theoretical uncertainties that we quantify to be as large as about one order of magnitude. We also discuss the positron fraction issue and find that our predictions may be consistent with the data taken before PAMELA. For PAMELA data, we find that an excess is probably present after considering uncertainties in the positron flux, although its amplitude depends strongly on the assumptions made in relation to the electron flux. By fitting the current electron data, we show that when considering a soft electron spectrum, the amplitude of the excess might be far lower than usually claimed. Conclusions. We provide fresh insights that may help to explain the positron data with or without new physical model ingredients. PAMELA observations and the forthcoming AMS-02 mission will allow stronger constraints to be aplaced on the cosmic-ray transport parameters, and are likely to reduce drastically the theoretical uncertainties.

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“…In principle, it could be included in the calculations using an iterative approach. Table 1: Galactic propagation models [9,10]. All models set R = 20 kpc.…”

Section: Antiproton Flux: the Conventional Formalismmentioning

confidence: 99%

Antiprotons from dark matter: Effects of a position-dependent diffusion coefficient

Perelstein

Shakya

2011

Phys. Rev. D

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Energetic antiprotons in cosmic rays can serve as an important indirect signature of dark matter. Conventionally, the antiproton flux from dark matter decay or annihilation is calculated by solving the transport equation with a space-independent diffusion coefficient within the diffusion zone of the galaxy. Antiproton sources outside the diffusion zone are ignored under the assumption that they propagate freely and escape. In reality, it is far more likely that the diffusion coefficient increases smoothly with distance from the disk, and the outlying part of the dark matter halo ignored in the conventional approach can be significant, containing as much as 90% of the galactic dark matter by mass in some models. We extend the conventional approach to address these issues. We obtain analytic approximations and numerical solutions for antiproton flux for a diffusion coefficient that increases exponentially with the distance from the disk, thereby including contributions from dark matter annihilation/decay in essentially the full dark matter halo. We find that the antiproton flux predicted in this model deviates from the conventional calculation for the same dark matter parameters by up to about 25%.

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Antiprotons in cosmic rays from neutralino annihilation

Cited by 362 publications

References 65 publications

DarkSUSY: computing supersymmetric dark matter properties numerically

DarkSUSY: computing supersymmetric dark matter properties numerically

Galactic secondary positron flux at the Earth

Antiprotons from dark matter: Effects of a position-dependent diffusion coefficient

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