A Numerical Study of Cosmic Proton Modulation Using AMS-02 Observations

Luo, Xi; Potgieter, M. S.; Bindi, V.; Zhang, Ming; Feng, Xueshang

doi:10.3847/1538-4357/ab1b2a

Cited by 25 publications

(13 citation statements)

References 76 publications

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“…As we have argued, the velocity factor β gives rise to little mass/charge dependence of CR diffusion in the lowrigidity limit, i.e., R 3 GV. Similar results were also reported by other authors (Corti et al, 2019;Boschini et al, 2019;Luo et al, 2019). In all these works, albeit based on different modeling, the conclusions are driven by the availability of new important measurements: the Voyager-1 data collected outside the heliosphere, and the AMS multi-channel and monthly-resolved data, collected locally and over a significant fraction of the Solar Cycle.…”

Section: Introductionsupporting

confidence: 83%

Numerical modeling of cosmic-ray transport in the heliosphere and interpretation of the proton-to-helium ratio in Solar Cycle 24

Tomassetti

Barão

Bertucci

et al. 2019

Advances in Space Research

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Thanks to space-borne experiments of cosmic-ray (CR) detection, such as the AMS and PAMELA missions in low-Earth orbit, or the Voyager-1 spacecraft in the interstellar space, a large collection of multi-channel and time-resolved CR data has become available. Recently, the AMS experiment has released new precision data, on the proton and helium fluxes in CRs, measured on monthly basis during its first six years of mission. The AMS data reveal a remarkable long-term behavior in the temporal evolution of the proton-to-helium ratio at rigidity R ≡ p/Z 3 GV. As we have argued in a recent work, such a behavior may reflect the transport properties of low-rigidity CRs in the inteplanetary space. In particular, it can be caused by mass/charge dependence of the CR diffusion coefficient. In this paper, we present our developments in the numerical modeling of CR transport in the Milky Way and in the heliosphere. Within our model, and with the help of approximated analytical solutions, we describe in details the relations between the properties of CR diffusion and the time-dependent evolution of the proton-to-helium ratio.

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Section: Introductionsupporting

confidence: 83%

Numerical modeling of cosmic-ray transport in the heliosphere and interpretation of the proton-to-helium ratio in Solar Cycle 24

Tomassetti

Barão

Bertucci

et al. 2019

Advances in Space Research

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“…Compared with previous works, we improve the technical treatments in several aspects to reduce potential uncertainties of the analyses. For the antiproton modeling, our novel treatment is to include the charge-sign-dependent three-dimensional (3D) solar modulation model [33,34] as constrained by the time-dependent AMS-02 proton data [35]. To investigate the GCE, taking a data-driven method, we identify the background components for the γ-ray sky solely with their spectral and morphological properties as in Ref.…”

Section: Introductionmentioning

confidence: 99%

Explaining the GeV antiproton/$γ-$ray excesses and W-boson mass anomaly in an inert two Higgs doublet model

Zhu¹,

Cui²,

Xia³

et al. 2022

Preprint

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For the newly discovered W-boson mass anomaly [1], one of the simplest dark matter (DM) models that can account for the anomaly without violating other astrophysical/experimental constraints is the inert two Higgs doublet model, in which the DM mass (m S ) is found to be within ∼ 54 − 74 GeV [2]. In this model, the annihilation of DM via S S → b b and S S → WW * would produce antiprotons and gamma rays, and may account for the excesses identified previously in both particles. Motivated by this, we re-analyze the AMS-02 antiproton and Fermi-LAT Galactic center gamma-ray data. For the antiproton analysis, the novel treatment is the inclusion of the charge-sign-dependent three-dimensional solar modulation model as constrained by the time-dependent proton data. We find that the excess of antiprotons is more distinct than previous results based on the forcefield solar modulation model. The interpretation of this excess as the annihilation of S S → WW * (S S → b b) requires a DM mass of ∼ 40−80 (40−60) GeV and a velocity-averaged cross section of O(10 −26 ) cm 3 s −1 . As for the γ-ray data analysis, rather than adopting the widely-used spatial template fitting, we employ an orthogonal approach with a data-driven spectral template analysis. The fitting to the GeV γ-ray excess yields DM model parameters overlapped with those to fit the antiproton excess via the WW * channel. The consistency of the DM particle properties required to account for the W-boson mass anomaly, the GeV antiproton excess, and the GeV γ-ray excess suggest a common origin of them.

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“…A similar report was made by le Roux & Potgieter (1995) who concluded that global merged interaction regions (GMIRS) forming beyond about 10 AU were required to reproduce the full amount of GCR modulation during 1977 to 1987. The effect of such a GMIR on AMS 02 proton observations was reported and modeled by Luo et al (2019). However, for the modulation period after 2009, it is not so obvious as after 1977 and 1987, how and when these GMIRS could have developed far beyond the Earth.…”

Section: Discussionmentioning

confidence: 99%

Time and Charge-Sign Dependence of the Heliospheric Modulation of Cosmic Rays

Aslam,

Bisschoff,

Ngobeni

et al. 2020

Preprint

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Simultaneous and continuous observations of galactic cosmic-ray electrons (e − ) and positrons (e + ) from the PAMELA and AMS 02 space experiments are most suitable for numerical modeling studies of the heliospheric modulation of these particles below 50 GeV. A well-established comprehensive three-dimensional (3D) modulation model is applied to compute full spectra for e − and e + with the purpose of reproducing the observed ratio e + /e − for a period which covers the previous long and unusual deep solar minimum activity and the recent maximum activity phase including the polarity reversal of the solar magnetic field. For this purpose the very local interstellar spectra for these particles were established first. Our study is focused on how the main modulation processes, including particle drifts, and other parameters such as the three major diffusion coefficients, had evolved, and how the corresponding charge-sign dependent modulation had occurred subsequently. The end result of our effort is the detailed reproduction of e + /e − from 2006 to 2015, displaying both qualitative and quantitative agreement with the main observed features. Particularly, we determine how much particle drifts is needed to explain the time dependence exhibited by the observed e + /e − during each solar activity phase, especially during the polarity reversal phase when no well-defined magnetic polarity was found.

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A Numerical Study of Cosmic Proton Modulation Using AMS-02 Observations

Cited by 25 publications

References 76 publications

Numerical modeling of cosmic-ray transport in the heliosphere and interpretation of the proton-to-helium ratio in Solar Cycle 24

Numerical modeling of cosmic-ray transport in the heliosphere and interpretation of the proton-to-helium ratio in Solar Cycle 24

Explaining the GeV antiproton/$γ-$ray excesses and W-boson mass anomaly in an inert two Higgs doublet model

Time and Charge-Sign Dependence of the Heliospheric Modulation of Cosmic Rays

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