{"arxiv_id":"0909.4548","incoming":{"papers":48,"sentences":62,"groups":[{"kind":"method_or_tool","label":"Uses its method or tool","papers":7,"sentences":7,"quotes":[{"arxiv_id":"1911.12977","title":"Positron Excess from Cosmic Ray Interactions in Galactic Molecular Clouds","url":"/paper/1911.12977","section":"Model setup","sentence":"In the present work, we study high energy CR propagation in our Galaxy, by solving the transport equation numerically, using publicly available code DRAGON[The 3D version of the DRAGON code is available at https://github.com/cosmicrays/DRAGON for download.] (Diffusion of cosmic RAys in Galaxy modelizatiON) [ref] .","intent_p":1.0,"contests_p":null},{"arxiv_id":"1506.05119","title":"The Galactic Center GeV Excess from a Series of Leptonic Cosmic-Ray Outbursts","url":"/paper/1506.05119","section":"Numerical simulations of outburst events","sentence":"To simulate the propagation of electrons in the GC and Inner Galaxy regions, we make use of the publicly available numerical codes [ref] and [ref] .","intent_p":1.0,"contests_p":null},{"arxiv_id":"2003.04700","title":"Impact of transport modelling on the $^{60}$Fe abundance inside Galactic cosmic ray sources","url":"/paper/2003.04700","section":"Transport model","sentence":"Notice that the spectrum has been corrected for the solar modulation using the widely used force-free approximation as in [ref] .","intent_p":0.98,"contests_p":null},{"arxiv_id":"1002.3341","title":"Pinpointing Cosmic Ray Propagation With The AMS-02 Experiment","url":"/paper/1002.3341","section":"Cosmic Ray Propagation in the Milky Way","sentence":"To proceed, one may either apply (semi-)analytical methods (e.g. [ref] ) or make use of numerical codes (e.g. GALPROP [ref] or DRAGON [ref] ).","intent_p":0.86,"contests_p":null},{"arxiv_id":"1110.4337","title":"Galactic synchrotron emission from WIMPs at radio frequencies","url":"/paper/1110.4337","section":"Synchrotron radiation","sentence":"This exponential dependence of the diffusion term on the cylindric coordinates is commonly adopted in numerical codes like Galprop [ref] and Dragon [ref] .","intent_p":0.86,"contests_p":null}]},{"kind":"data_used","label":"Uses its data or values","papers":1,"sentences":1,"quotes":[{"arxiv_id":"1410.4842","title":"Galactic Centre GeV Photons from Dark Technicolor","url":"/paper/1410.4842","section":"Introduction","sentence":"In addition, it has been noted that data from the PAMELA experiment [ref] exhibit a 40% excess of antiprotons in the 1-3 GeV energy range over expectations from cosmic ray propagation models [ref] .","intent_p":0.83,"contests_p":null}]},{"kind":"comparison","label":"Compares with it","papers":3,"sentences":3,"quotes":[{"arxiv_id":"1002.3341","title":"Pinpointing Cosmic Ray Propagation With The AMS-02 Experiment","url":"/paper/1002.3341","section":"Constraining propagation models","sentence":"This precision is much greater than that obtained with present (pre-AMS-02) data; see Refs. [ref] .","intent_p":0.87,"contests_p":null},{"arxiv_id":"1504.05175","title":"Secondary antiprotons as a Galactic Dark Matter probe","url":"/paper/1504.05175","section":"Discussion on AMS-02 data","sentence":"It is worth noting here that the $δ$ required by the new high-energy measurements is in perfect agreement with the best-fit value obtained in our earlier statistical analysis [ref] , based on the available high-energy measurements preceding PAMELA and AMS-02 releases.","intent_p":0.83,"contests_p":null},{"arxiv_id":"1210.4546","title":"Cosmic Ray Electrons, Positrons and the Synchrotron emission of the Galaxy: consistent analysis and implications","url":"/paper/1210.4546","section":"Back to the $e^+$ and $e^-$ observed spectra","sentence":"We notice that the KRA model in [ref] , though similar to its homologous in this paper, reproduced the positron fraction measured by PAMELA down to $1$ rather than that of 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.","intent_p":0.96,"contests_p":null},{"arxiv_id":"2005.04237","title":"Dark matter or correlated errors: Systematics of the AMS-02 antiproton excess","url":"/paper/2005.04237","section":"Cosmic-ray production and propagation","sentence":"This change is partly motivated by recent studies [ref] which observed a substantial improvement in the fit to secondary nuclear cosmic rays within the diffusion model with free $η$.","intent_p":1.0,"contests_p":null}]},{"kind":"background","label":"Cites it as background","papers":7,"sentences":7,"quotes":[{"arxiv_id":"1101.5524","title":"Galactic Magnetic Turbulence from Radio data","url":"/paper/1101.5524","section":"Results and Discussion","sentence":"If data are interpreted assuming a low convection wind (i.e., null or linearly increasing in the vertical direction), ratios of secondaries to primaries can be typically well-fitted by diffusion (plus reacceleration) models with Kolmogorov ($γ=1/3$) [ref] or Kraichnan ($γ=1/2$) [ref] spectrum of turbulence.","intent_p":0.89,"contests_p":null},{"arxiv_id":"1012.0587","title":"Antiproton Flux in Cosmic Ray Propagation Models with Anisotropic Diffusion","url":"/paper/1012.0587","section":"Introduction","sentence":"These include both semi-analytic [ref] as well as fully numerical treatments [ref] .","intent_p":0.85,"contests_p":null},{"arxiv_id":"2303.07362","title":"Fast and accurate AMS-02 antiproton likelihoods for global dark matter fits","url":"/paper/2303.07362","section":"Choice of models","sentence":"The INJ.BRK (injection break) model has been explored extensively in literature [ref] .","intent_p":0.97,"contests_p":null},{"arxiv_id":"2406.18642","title":"$\\overline{\\text{D}}$arkRayNet: Emulation of cosmic-ray antideuteron fluxes from dark matter","url":"/paper/2406.18642","section":"Propagation","sentence":"This model has been extensively studied in the literature [ref] .","intent_p":0.92,"contests_p":null},{"arxiv_id":"1510.04623","title":"Production of secondary 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.","intent_p":0.9,"contests_p":null},{"arxiv_id":"astro-ph/0002481","title":"Precise Measurement of Cosmic-Ray Proton and Helium Spectra with the BESS Spectrometer","url":"/paper/astro-ph/0002481","section":"Solar modulation","sentence":"For protons and antiprotons we use a potential which allows to match BESS98 [ref] , AMS-01 [ref] and PAMELA [ref] proton data even well below 1 GeV/n (see Fig. [ref]).","intent_p":0.96,"contests_p":null},{"arxiv_id":"astro-ph/0410214","title":"The solar chemical composition","url":"/paper/astro-ph/0410214","section":"Target gas","sentence":"Following [ref] we take the He/H numerical fraction in the ISM to be 0.11.","intent_p":1.0,"contests_p":null}]},{"kind":"comparison","label":"Compares with","papers":6,"sentences":11,"quotes":[{"arxiv_id":"astro-ph/0406254","title":"Diffuse Galactic continuum gamma rays. A model compatible with EGRET data and cosmic-ray measurements","url":"/paper/astro-ph/0406254","section":"Discussion and comparison with previous results","sentence":"In order to clarify the reasons of such a discrepancy, in Fig. [ref] and [ref] we compare the predictions of our reference diffusion-reacceleration model $(δ, D_0/z_t, v_A, η) = (0.5, 0.7, 15, - 0.4)$, which for brevity we call Kraichnan model, with those obtained using the propagation parameters (and source distribution) of the Kolmogorov model discussed in [ref] , namely $(δ, D_0(4 GV)/z_t, v_A, η) = (0.33,1.45, 30, 1)$ [In [ref] a spatially uniform diffusion coefficient ($z_t=z_max = 4$) was assumed.","intent_p":0.98,"contests_p":null},{"arxiv_id":"astro-ph/0101231","title":"Cosmic Rays below Z=30 in a diffusion model: new constraints on propagation parameters","url":"/paper/astro-ph/0101231","section":"Discussion and comparison with previous results","sentence":"In spite of these differences, and that CREAM and PAMELA data were not included in those analyses for chronological reasons, it is comforting that for low values of the convective velocity $v_c ≃0$ the preferred value of $δ$ estimated in [ref] is in remarkably good agreement with that found in this work: $δ≃0.45$.","intent_p":1.0,"contests_p":null},{"arxiv_id":"astro-ph/0206286","title":"New results on source and diffusion spectral features of Galactic cosmic rays: I- B/C ratio","url":"/paper/astro-ph/0206286","section":"Discussion and comparison with previous results","sentence":"In spite of these differences, and that CREAM and PAMELA data were not included in those analyses for chronological reasons, it is comforting that for low values of the convective velocity $v_c ≃0$ the preferred value of $δ$ estimated in [ref] is in remarkably good agreement with that found in this work: $δ≃0.45$.","intent_p":1.0,"contests_p":null},{"arxiv_id":"astro-ph/0510335","title":"Dissipation of Magnetohydrodynamic Waves on Energetic Particles: Impact on Interstellar Turbulence and Cosmic Ray Transport","url":"/paper/astro-ph/0510335","section":"A comprehensive model describing all data sets down to $0.1 /n$","sentence":"Interestingly, the value of $δ$ used in [ref] to fit the B/C in the presence of MHD wave dissipation is 0.5, which is consistent with what we found here (differently from what we do here, however, a break in the injection index was invoked in that work).","intent_p":0.89,"contests_p":null},{"arxiv_id":"astro-ph/0212111","title":"Galactic Cosmic Ray Nuclei as a Tool for Astroparticle Physics","url":"/paper/astro-ph/0212111","section":"Cosmic ray sources","sentence":"This is slightly different from the radial distributions adopted in [ref] and in [ref] which are based on pulsar surveys only.","intent_p":0.97,"contests_p":null}]},{"kind":"supports_this_paper","label":"Cites as support","papers":1,"sentences":1,"quotes":[{"arxiv_id":"0807.4730","title":"Cosmic-Ray Nuclei, Antiprotons and Gamma-rays in the Galaxy: a New Diffusion Model","url":"/paper/0807.4730","section":"Spatial diffusion coefficient","sentence":"As shown in [ref] , a vertically growing $D$ is physically more realistic than a uniform one and allows to get a more regular behavior of the CR density at the vertical boundaries of the propagation halo with respect to the case of uniform diffusion.","intent_p":0.97,"contests_p":null}]},{"kind":"background","label":"Cites as background","papers":14,"sentences":15,"quotes":[{"arxiv_id":"astro-ph/0701517","title":"Cosmic-ray propagation and interactions in the Galaxy","url":"/paper/astro-ph/0701517","section":"Introduction","sentence":"Well known realizations of these two approaches are respectively the two-zone model (see e.g. [ref] ) and the GALPROP package [ref] .","intent_p":0.9,"contests_p":null},{"arxiv_id":"astro-ph/0101231","title":"Cosmic Rays below Z=30 in a diffusion model: new constraints on propagation parameters","url":"/paper/astro-ph/0101231","section":"Introduction","sentence":"Well known realizations of these two approaches are respectively the two-zone model (see e.g. [ref] ) and the GALPROP package [ref] .","intent_p":0.9,"contests_p":null},{"arxiv_id":"astro-ph/0206286","title":"New results on source and diffusion spectral features of Galactic cosmic rays: I- B/C ratio","url":"/paper/astro-ph/0206286","section":"Introduction","sentence":"Well known realizations of these two approaches are respectively the two-zone model (see e.g. [ref] ) and the GALPROP package [ref] .","intent_p":0.9,"contests_p":null},{"arxiv_id":"astro-ph/0212111","title":"Galactic Cosmic Ray Nuclei as a Tool for Astroparticle Physics","url":"/paper/astro-ph/0212111","section":"Introduction","sentence":"Well known realizations of these two approaches are respectively the two-zone model (see e.g. [ref] ) and the GALPROP package [ref] .","intent_p":0.9,"contests_p":null},{"arxiv_id":"astro-ph/0406254","title":"Diffuse Galactic continuum gamma rays. 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