## Despite significant efforts over the last decade, the origin of the cosmic ray positron excess has still not been unambiguously established. 尽管在过去十年中做出了重大努力，但宇宙射线正电子过剩的起源仍未明确确定。

Explaining cosmic ray antimatter with secondaries from old supernova remnants

## In this contribution we present a detailed study of the GeV gamma-ray halo around Geminga and Monogem, and show the constraints found for the contribution of these PWNe to the cosmic-ray positron excess, combining Milagro and HAWC data with measurements from the Fermi-LAT for the first time. nan

Detection of a gamma-ray halo around Geminga with the Fermi-LAT and implications for the positron flux

## We revisit dark matter annihilation as an explanation of the positron excess reported recently by the AMS-02 satellite-borne experiment. 我们重新审视暗物质湮灭作为对 AMS-02 星载实验最近报告的正电子过剩的解释。

Leptophilic-portal dark matter in the light of AMS-02 positron excess

## This has important implication for the interpretation of the CR positron excess. 这对解释 CR 正电子过剩具有重要意义。

Test of the superdiffusion model in the interstellar medium around the Geminga pulsar

## This is called ‘positron excess’ whose origin remains unknown, and interpretations including supernova remnants, pulsar wind nebulae (PWNe) or dark matter have been considered. 这被称为“正电子过剩”，其起源仍然未知，包括超新星遗迹、脉冲风星云 (PWNe) 或暗物质在内的解释已经被考虑在内。

Emission of cosmic rays from Pulsar wind nebulae

## Sommerfeld-enhanced dark matter (DM) annihilation through s-wave has been widely considered as a consistent explanation for both the observed cosmic-ray (CR) positron excess and the DM thermal relic density. Sommerfeld 增强的 s 波暗物质 (DM) 湮没已被广泛认为是观测到的宇宙射线 (CR) 正电子过剩和 DM 热遗迹密度的一致解释。

Consistent explanation for the cosmic-ray positron excess in p-wave Sommerfeld-enhanced dark matter annihilation

## In this paper, we instead examine the potential for extremely precise positron measurements by AMS-02 to probe hard leptophilic dark matter candidates that do not have spectral features similar to the bulk of the observed positron excess. 在本文中，我们改为研究 AMS-02 进行极其精确的正电子测量以探测不具有与观察到的大部分正电子过剩相似的光谱特征的硬亲亲暗物质候选者的潜力。

Cosmic-Ray Positrons Strongly Constrain Leptophilic Dark Matter

## Despite significant efforts over the last decade, the origin of the cosmic ray positron excess has still not been unambiguously established. 尽管在过去十年中做出了重大努力，但宇宙射线正电子过剩的起源仍未明确确定。

Explaining cosmic ray antimatter with secondaries from old supernova remnants

## In particular, the AMS-02 anti-proton and positron excesses have continued to grow more robust with the collection of more data.

An excess of excesses examined via dark matter radio emissions from galaxies

## As a consequence, the most likely pulsar source of the positron excess, Geminga, is no more a viable candidate under the additional constraint from Fermi-LAT.

Reanalyze the pulsar scenario to explain the cosmic positron excess considering the recent developments

## With experimental results of AMS on the spectra of cosmic ray (CR) $e^{-}$, $e^{+}$, $e^{-}+e^{+}$ and positron fraction, as well as new measurements of CR $e^{-}+e^{+}$ flux by HESS, one can better understand the CR lepton ($e^{-}$ and $e^{+}$) spectra and the puzzling electron-positron excess above $\sim$10 GeV.

Origin of Cosmic Ray Electrons and Positrons

## This result also constrains the modeling of the positron excesses.

Overview of Direct Measurements of Cosmic Rays

## Our results are compatible with the interpretation that the cumulative emission from Galactic pulsars explains the positron excess.

Detection of a γ -ray halo around Geminga with the Fermi-LAT data and implications for the positron flux

## One possible explanation can be that positron excess is generated by ~ TeV dark matter particles annihilation or decay.

Method of positron detection using the Earth magnetic field in orbital experiment

## It includes effects in cosmic rays (CR): first of all, the positron excess at $\sim$ 500 GeV and possible electron-positron excess at 1-1.

Indirect effects of dark matter

## Our findings must be reckoned with theories of Galactic CR transport, which often assume that electrons and protons are injected with the same slope, and may especially have implications for the observed "positron excess".

Spectrum of Electrons Accelerated in Supernova Remnants.

## The positron excess observed by PAMELA and then confirmed by AMS 02 has intrigued the particle physics community since 2008.

Dark matter decaying into millicharged particles as a solution to AMS-02 positron excess

## Recent (and earlier) analyses of the data from Planck, Fermi-LAT, AMS-02, and other experiments indicate that (i) the positron excess at ∼ 800 GeV or above is not evidence of highmass dark matter particles (which would have disconfirmed the present theory with a rigorous upper limit of 125 GeV), (ii) the Galactic center excess of gamma rays observed by Fermi is evidence for dark matter particles with a mass below or near 100 GeV, (iii) the gamma-ray excess from Omega Centauri is similar evidence of annihilation of such relatively low-mass particles, and (iv) the antiproton excess observed by AMS is again evidence of.

P 2 0 1 9 ) 0 9 9 A multicomponent dark matter scenario and the experimental evidence supporting it

## By modeling the TeV emission as inverse Compton emission from electron-positron pairs diffusing in the interstellar medium (ISM), the HAWC collaboration derives a diffusion coefficient much smaller than the standard value in the vicinity of the two pulsars, which make them unlikely the origin of the positron excess.

Positron flux and γ-ray emission from Geminga pulsar and pulsar wind nebula

## We study the gauged $U(1)_{L_\mu-L_\tau}$ scotogenic model with emphasis on latest measurement of LHCb $R_{K^{(*)}}$ anomaly and AMS-02 positron excess.

Gauged $U(1)_{L_\mu-L_\tau}$ Scotogenic Model in light of $R_{K^{(*)}}$ Anomaly and AMS-02 Positron Excess

## In the light of the latest measurements on the total $e^+ + e^-$ flux by CALET and DAMPE experiments, we revisit the multicomponent leptonically decaying dark matter (DM) explanations to the cosmic-ray electron/positron excesses observed previously.

Multicomponent Dark Matter in the Light of CALET and DAMPE

## After including these GMCs we show that the positron excess can be mostly well explained, with a small contribution from unknown extra component near the peak.

Positron Excess from Cosmic Ray Interactions in Galactic Molecular Clouds

## With experimental results of AMS on the spectra of cosmic ray (CR) e^−, e^+, e^− + e^+ and positron fraction, as well as new measurements of CR e^− + e^+ flux by HESS, one can better understand the CR lepton (e^− and e^+) spectra and the puzzling electron–positron excess above ∼10 GeV.

Origin of Cosmic Ray Electrons and Positrons

## In this contribution we present a detailed study of the GeV gamma-ray halo around Geminga and Monogem, and show the constraints found for the contribution of these PWNe to the cosmic-ray positron excess, combining Milagro and HAWC data with measurements from the Fermi-LAT for the first time.

Detection of a gamma-ray halo around Geminga with the Fermi-LAT and implications for the positron flux