Propagation of cosmic rays in the AMS-02 era

Yuan, Qiang; Lin, Su-Jie; Fang, Kun; Bi, Xiao-Jun

doi:10.1103/physrevd.95.083007

Cited by 119 publications

(161 citation statements)

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“…As for the modulation potential, we employ a time-variation form Φ = Φ 0 + Φ 1 ×Ñ(t) to connect the modulation with solar activities which are characterized by the sunspot number 2Ñ (t) (normalized to 1 at solar maximum of cycle 24). The data used in the fitting include the B/C data by ACE [31] and AMS-1 Other propagation scenarios, such as the plain diffusion and diffusion convection models, have also been discussed in [26]. However, the diffusion reacceleration scenario is found to be best consistent with the data.…”

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confidence: 49%

“…With these data, we conduct a global study to determine the propagation, injection, and solar modulation parameters si- * The corresponding author: yuanq@pmo.ac.cn † The corresponding author: yzfan@pmo.ac.cn multaneously using the Markov Chain Monte Carlo (MCMC) method [26]. These "background" parameters and their likelihoods can be incorporated in the study of the DM model parameters by means of the Bayesian theorem, giving selfconsistent and unbiased judgement of the DM models (see earlier attempts [17,23]).…”

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confidence: 99%

“…Note, however, we adopt a relatively simple one-zone diffusion model in this work. It is possible that in reality the ISM and CR propagation are more complicated, e.g., vary everywhere [25].Background -Here we simply introduce the fitting procedure to determine the propagation, injection, and solar modulation parameters [26,28]. Hereafter they are referred to as background parameters.…”

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confidence: 99%

“…Background -Here we simply introduce the fitting procedure to determine the propagation, injection, and solar modulation parameters [26,28]. Hereafter they are referred to as background parameters.…”

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confidence: 99%

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Possible Dark Matter Annihilation Signal in the AMS-02 Antiproton Data

et al. 2017

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Using the latest AMS-02 cosmic ray antiproton flux data, we search for potential dark matter annihilation signal. The background parameters about the propagation, source injection, and solar modulation are not assumed a priori, but based on the results inferred from the recent B/C ratio and proton data measurements instead. The possible dark matter signal is incorporated into the model self-consistently under a Bayesian framework. Compared with the astrophysical background only hypothesis, we find that a dark matter signal is favored. The rest mass of the dark matter particles is ∼ 20 − 80 GeV and the velocity-averaged hadronic annihilation cross section is about (0.2 − 5) × 10 −26 cm 3 s −1 , in agreement with that needed to account for the Galactic center GeV excess and/or the weak GeV emission from dwarf spheroidal galaxies Reticulum 2 and Tucana III. Tight constraints on the dark matter annihilation models are also set in a wide mass region. PACS numbers: 95.35.+d,Introduction -The precise measurements of cosmic ray (CR) anti-particle spectra by space-borne instruments, such as PAMELA and AMS-02, provide very good sensitivity to probe the particle dark matter (DM) annihilation or decay in the Milky Way. The CR antiprotons, primarily come from the inelastic collisions between the CR protons (and Helium) and the interstellar medium (ISM), are effective to constrain the DM models [1][2][3]. Recent observations of the antiproton fluxes [4][5][6] are largely consistent with the expectation from the CR propagation model, leaving very limited room for the annihilation or decay of DM [2,[7][8][9][10].There are several sources of uncertainties in using antiprotons to constrain DM models. The largest uncertainty may come from the propagation parameters. Usually the secondary-to-primary ratio of CR nuclei, such as the Boronto-Carbon ratio (B/C), and the radioactive-to-stable isotope ratio of secondary nuclei, such as the Beryllium isotope ratio 10 Be/ 9 Be, are used to determine the propagation parameters [11,12]. Limited by the data quality, the constraints on the propagation parameters are loose [13,14]. Even the effect on the background antiproton flux due to uncertainties of propagation parameters is moderate, the flux from the DM component depends sensitively on propagation parameters [15]. Additional uncertainties include the injection spectrum of the CR nuclei, solar modulation, and hadronic interaction models [8]. Those uncertainties make the DM searches with antiprotons inconclusive [16,17].Given the new measurements of the proton, Helium, and B/C data by , improved constraints on the propagation and source injection parameters can be obtained through global Bayesian approaches [22][23][24][25]. With these data, we conduct a global study to determine the propagation, injection, and solar modulation parameters si- * The corresponding author: yuanq@pmo.ac.cn † The corresponding author: yzfan@pmo.ac.cn multaneously using the Markov Chain Monte Carlo (MCMC) method [26]. These "background" parameters and their like...

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confidence: 49%

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confidence: 99%

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confidence: 99%

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Possible Dark Matter Annihilation Signal in the AMS-02 Antiproton Data

et al. 2017

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“…where r = 8.5 kpc is the distance between the Sun and the Galactic center [33], the height of the Galactic disk is z s = 0.2 kpc. The two parameters a and b are chosen to be 1.25 and 3.56, respectively [34].…”

Section: Antiproton Flux From Ams-02mentioning

confidence: 99%

Revisiting simplified dark matter models in terms of AMS-02 and Fermi-LAT

2018

J. High Energ. Phys.

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Abstract:We perform an analysis of the simplified dark matter models in the light of cosmic ray observables by AMS-02 and Fermi-LAT. We assume fermion, scalar or vector dark matter particle with a leptophobic spin-0 mediator that couples only to Standard Model quarks and dark matter via scalar and/or pseudo-scalar bilinear. The propagation and injection parameters of cosmic rays are determined by the observed fluxes of nuclei from AMS-02. We find that the AMS-02 observations are consistent with the dark matter framework within the uncertainties. The AMS-02 antiproton data prefer 30 (50) GeV -5 TeV dark matter mass and require an effective annihilation cross section in the region of 4 × 10 −27 (7 × 10 −27 ) -4 × 10 −24 cm 3 /s for the simplified fermion (scalar and vector) dark matter models. The cross sections below 2 × 10 −26 cm 3 /s can evade the constraint from Fermi-LAT dwarf galaxies for about 100 GeV dark matter mass.

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Explanations of the DAMPE high energy electron/positron spectrum in the dark matter annihilation and pulsar scenarios

Wang

Lin

et al. 2018

Sci. China Phys. Mech. Astron.

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Many studies have shown that either the nearby astrophysical source or dark matter (DM) annihilation/decay is required to explain the origin of high energy cosmic ray (CR) e ± , which are measured by many experiments, such as PAMELA and AMS-02. Recently, the Dark Matter Particle Explorer (DAMPE) collaboration has reported its first result of the total CR e ± spectrum from 25 GeV to 4.6 TeV with high precision. In this work, we study the DM annihilation and pulsar interpretations of the DAMPE high energy e ± spectrum. In the DM scenario, the leptonic annihilation channels to τ + τ − , 4µ, 4τ , and mixed charged lepton final states can well fit the DAMPE result, while the µ + µ − channel has been excluded. In addition, we find that the mixed charged leptons channel would lead to a sharp drop at ∼ TeV. However, these DM explanations are almost excluded by the observations of gamma-ray and CMB, unless some complicated DM models are introduced. In the pulsar scenario, we analyze 21 nearby known pulsars and assume that one of them is the primary source of high energy CR e ± . Considering the constraint from the Fermi-LAT observation of the e ± anisotropy, we find that two pulsars are possible to explain the DAMPE data. Our results show that it is difficult to distinguish between the DM annihilation and single pulsar explanations of high energy e ± with the current DAMPE result.

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Propagation of cosmic rays in the AMS-02 era

Cited by 119 publications

References 80 publications

Possible Dark Matter Annihilation Signal in the AMS-02 Antiproton Data

Possible Dark Matter Annihilation Signal in the AMS-02 Antiproton Data

Revisiting simplified dark matter models in terms of AMS-02 and Fermi-LAT

Explanations of the DAMPE high energy electron/positron spectrum in the dark matter annihilation and pulsar scenarios

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