# GeV-TeV Cosmic Ray Leptons in the Solar System from the Bow Shock Wind Nebula of the Nearest Millisecond Pulsar J0437-4715

## TL;DR

This paper models how leptons accelerated in the bow shock nebula of pulsar J0437-4715 can explain observed positron excesses and high-energy lepton fluxes in the Solar System, linking astrophysical acceleration processes to cosmic ray observations.

## Contribution

It presents a new model connecting pulsar nebula acceleration with observed cosmic ray leptons and positron excesses in the Solar System.

## Key findings

- Leptons from the nebula can account for positron fraction increase above a few GeV.
- Model spectra match ultraviolet and X-ray observations of the nebula.
- Accelerated leptons can explain TeV-range lepton fluxes observed by multiple detectors.

## Abstract

We consider acceleration of leptons up to GeV-TeV energies in the bow shock wind nebula of PSR J0437-4715 and their subsequent diffusion through the interstellar magnetic fields. The leptons accelerated at the pulsar wind termination surface are injected into re-acceleration in colliding shock flows. Modelled spectra of synchrotron emission from the accelerated electrons and positrons are consistent with the far-ultraviolet and X-ray observations of the nebula carried out with the Hubble Space Telescope and Chandra X-ray Observatory. These observations are employed to constrain the absolute fluxes of relativistic leptons, which are escaping from the nebula and eventually reaching the Solar System after energy-dependent diffusion through the local interstellar medium accompanied by synchrotron and Compton losses. It is shown that accelerated leptons from the nebula of PSR J0437-4715 can be responsible both for the enhancement of the positron fraction above a few GeV detected by PAMELA and AMS-02 spectrometers and for the TeV range lepton fluxes observed with H.E.S.S., VERITAS, Fermi, CALET, and DAMPE.