Constraining the Diffusion Coefficient with HAWC TeV Gamma-Ray Observations of Two Nearby Pulsar Wind Nebulae

TL;DR

This study uses HAWC gamma-ray observations of two nearby pulsar wind nebulae to constrain the diffusion coefficient of high-energy particles in our galaxy, providing insights into cosmic ray propagation.

Contribution

It presents a new model and morphological analysis of two PWNe to derive the diffusion coefficient at TeV energies, based on HAWC data.

Findings

Derived diffusion coefficient constraints from HAWC observations.

Morphological analysis supports specific diffusion models.

Provides improved understanding of particle propagation near PWNe.

Abstract

Nearby electron/positron accelerators, mostly Pulsar Wind Nebulae (PWNe), have been proposed as potential origins of the positron excess above 10 GeV. The HAWC Observatory reveals two very extended sources spatially coincident with two nearby middle-aged pulsars: Geminga and PSR B0656+14, suggesting ultrarelativistic electrons/positrons accelerated in our backyard. Morphological studies on these two PWNe provide a constraint on the diffusion coefficient at HAWC energies. In this poster, we will present the model development and morphological studies on these PWNe, and the derived diffusion coefficient that best fits the data.