Pulsar wind zone processes in LS 5039

TL;DR

This paper develops a detailed theoretical model of gamma-ray binaries with pulsars, focusing on system geometry, radiation processes, and cascades, to explain observed high-energy emissions, exemplified by LS 5039.

Contribution

It provides a comprehensive, detailed model including geometry, anisotropic processes, and cascades, specifically applied to LS 5039, advancing understanding of pulsar wind zone processes in gamma-ray binaries.

Findings

Model matches H.E.S.S. observations of LS 5039

Highlights importance of pulsar wind zone opacities

Analyzes shock position impact on emissions

Abstract

Several $\gamma$-ray binaries have been recently detected by the High-Energy Stereoscopy Array (H.E.S.S.) and the Major Atmospheric Imaging Cerenkov (MAGIC) telescope. In at least two cases, their nature is unknown. In this paper we aim to provide the details of a theoretical model of close $\gamma$-ray binaries containing a young energetic pulsar as compact object, earlier presented in recent Letters. This model includes a detailed account of the system geometry, the angular dependence of processes such as Klein-Nishina inverse Compton and $\gamma\gamma$ absorption in the anisotropic radiation field of the massive star, and a Monte Carlo simulation of leptonic cascading. We present and derive the used formulae and give all details about their numerical implementation, particularly, on the computation of cascades. In this model, emphasis is put in the processes occurring in the pulsar wind zone of the binary, since, as we show, opacities in this region can be already important for close systems. We provide a detailed study on all relevant opacities and geometrical dependencies along the orbit of binaries, exemplifying with the case of LS 5039. This is used to understand the formation of the very high-energy lightcurve and phase dependent spectrum. For the particular case of LS 5039, we uncover an interesting behavior of the magnitude representing the shock position in the direction to the observer along the orbit, and analyze its impact in the predictions. We show that in the case of LS 5039, the H.E.S.S. phenomenology is matched by the presented model, and explore the reasons why this happens while discussing future ways of testing the model.