Possible bump structure of cosmic ray electrons unveiled by AMS-02 data and its common origin along with the nuclei and positron

TL;DR

This paper proposes that a common local source, such as Geminga pulsar and SNR, explains the observed high-energy excesses of positrons, electrons, and nuclei, predicting a detectable bump in the electron spectrum above 284 GeV.

Contribution

It introduces a unified model linking positron, electron, and nuclei excesses to a single local source, supported by spatially-dependent propagation simulations.

Findings

A sharp electron bump above 284 GeV is necessary to fit AMS-02 data.

The model successfully reproduces positron, electron, and nuclei excesses from a common source.

Future AMS-02 observations could confirm the predicted bump structure.

Abstract

The local pulsar and its progenitor, SNR, can together accelerate the positron, electron and nuclei to very high energy. The famous excesses of positron(nuclei) above $20$($200$) GeV possibly come from such kind of local source. This hints that the primary electron should also hold "excess" above $200$ GeV, synchronously accelerated along with the nuclei. The recent precise measurement of sharp dropoff at 284 GeV of positron by AMS-02 experiment takes chance to study this expected electron excess. In this work, the spatially-dependent propagation with a local source is used to reproduce the spectrum of positron, electron and proton. When considering the dropoff at 284 GeV of positron, a sharp bump structure for primary electron above 284 GeV is required to fit the total spectrum of positron and electron. Then we systematically study the common origin of the excesses of positron, electron and nuclei from Geminga pulsar and SNR. Those excesses can be reproduced under this unified single-source model. Lastly, we hope that the fine bump structure can be observed to support our model by AMS-02 experiment in future.