Propagation of Cosmic‐Ray Nucleons in the Galaxy

Strong, A. W.; Moskalenko, I. V.

doi:10.1086/306470

Cited by 1,048 publications

(1,294 citation statements)

References 48 publications

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“…Also , for antiprotons [96] and antideuterons we neglect energy losses (whenever a scattering with a nucleus takes place the particle is removed), while for positrons [97] we consider an average over space of the energy loss effect due to inverse Compton on starlight and the cosmic microwave background, and in addition the synchrotron radiation from the effects of the galactic magnetic field. For comparison, we allow also the option to treat the propagation of antiprotons according to the propagation models by Chardonnet et al [94] and Bottino et al [95], while for the positron we have implemented the option to use the leaky-box treatment given by Kamionkowski and Turner [93] or the numerical Green functions derived by Moskalenko and Strong [106] with the Galprop code [105] (the latter two cases however cannot be interfaced to a generic axisymmetric dark matter density profile, as for our default propagation model).…”

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.

907

1,058

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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.

907

1,058

View full text Add to dashboard Cite

show abstract

“…This kind of numerical method has been adopted for the solution of the transport equation in the Milky Way, e.g., by the publicly available codes GALPROP (Strong & Moskalenko 1998) and DRAGON (Evoli et al 2008). The main differences in our case are that we have a 2D propagation (in r and E) due to the spherical symmetry (instead of 3D or 4D as for the Galaxy) and we consider a logarithmic scale for the spatial grid.…”

Section: Appendix A: Solution For Spherically-symmetric Transport Equmentioning

confidence: 99%

Local Group dSph radio survey with ATCA – II. Non-thermal diffuse emission

Regis

Richter

Colafrancesco

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Our closest neighbours, the Local Group dwarf spheroidal (dSph) galaxies, are extremely quiescent and dim objects, where thermal and non-thermal diffuse emissions lack, so far, of detection. In order to possibly study the dSph interstellar medium, deep observations are required. They could reveal non-thermal emissions associated with the very-low level of star formation, or to particle dark matter annihilating or decaying in the dSph halo. In this work, we employ radio observations of six dSphs, conducted with the Australia Telescope Compact Array in the frequency band 1.1-3.1 GHz, to test the presence of a diffuse component over typical scales of few arcmin and at an rms sensitivity below 0.05 mJy/beam. We observed the dSph fields with both a compact array and long baselines. Short spacings led to a synthesized beam of about 1 arcmin and were used for the extended emission search. The high-resolution data mapped background sources, which in turn were subtracted in the short-baseline maps, to reduce their confusion limit. We found no significant detection of a diffuse radio continuum component. After a detailed discussion on the modelling of the cosmic-ray (CR) electron distribution and on the dSph magnetic properties, we present bounds on several physical quantities related to the dSphs, such that the total radio flux, the angular shape of the radio emissivity, the equipartition magnetic field, and the injection and equilibrium distributions of CR electrons. Finally, we discuss the connection to far-infrared and X-ray observations.

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“…The GALPROP numerical package is by far the most developed tool for consistent cosmic-ray analysis [54,55]. The code solves a network of transport equations for Z≥1 nuclei as well as for electrons and positrons while computing energy losses using realistic maps of galactic gas [56] and of the far-infrared, optical and CMB photons that make up the Inter-Stellar Radiation Field (ISRF) [57].…”

Section: Consistent Modeling Of the High-energy Skymentioning

confidence: 99%

“…As δ describes the spectrum of turbulent features in the bulk magnetic field, there has been a large industry devoted to theoretical and experimental considerations of what its value should be [68][69][70][71][72][73]. Particularly well-motivated theoretical values include δ = 0.33 (Kolmogorov turbulence) and δ = 0.5 (Kraichnan turbulence).…”

Section: Jhep01(2011)064mentioning

confidence: 99%

Cosmic ray anomalies from the MSSM?

Cotta

Conley

Gainer

et al. 2011

J. High Energ. Phys.

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Abstract:The recent positron excess in cosmic rays (CR) observed by the PAMELA satellite may be a signal for dark matter (DM) annihilation. When these measurements are combined with those from FERMI on the total (e + + e − ) flux and from PAMELA itself on thep/p ratio, these and other results are difficult to reconcile with traditional models of DM, including the conventional mSUGRA version of Supersymmetry even if boosts as large as 10 3−4 are allowed. In this paper, we combine the results of a previously obtained scan over a more general 19-parameter subspace of the MSSM with a corresponding scan over astrophysical parameters that describe the propagation of CR. We then ascertain whether or not a good fit to this CR data can be obtained with relatively small boost factors while simultaneously satisfying the additional constraints arising from gamma ray data. We find that a specific subclass of MSSM models where the LSP is mostly pure bino and annihilates almost exclusively into τ pairs comes very close to satisfying these requirements. The lightestτ in this set of models is found to be relatively close in mass to the LSP and is in some cases the nLSP. These models lead to a significant improvement in the overall fit to the data by an amount ∆χ 2 ∼ 1/dof in comparison to the best fit without Supersymmetry while employing boosts ∼ 100. The implications of these models for future experiments are discussed.

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Propagation of Cosmic‐Ray Nucleons in the Galaxy

Cited by 1,048 publications

References 48 publications

DarkSUSY: computing supersymmetric dark matter properties numerically

DarkSUSY: computing supersymmetric dark matter properties numerically

Local Group dSph radio survey with ATCA – II. Non-thermal diffuse emission

Cosmic ray anomalies from the MSSM?

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