Gamma-ray spectral properties of mature pulsars: a two-layer model

TL;DR

This paper presents a two-layer outer gap model for mature pulsars to explain their gamma-ray spectra, showing how gap parameters influence spectral features and luminosity, with implications for understanding pulsar emission mechanisms.

Contribution

The paper introduces a simplified two-layer outer gap model that links gap parameters to gamma-ray spectral properties and luminosity in mature pulsars, providing new insights into their emission processes.

Findings

Gamma-ray spectra can deviate from simple curvature radiation due to two-component emission.

Fractional gap thickness increases with pulsar age.

Gamma-ray luminosity's dependence on spin-down power varies with luminosity level.

Abstract

We use a simple two-layer outer gap model, whose accelerator consists of a primary region and a screening region, to discuss $\gamma$-ray spectrum of mature pulsars detected by $Fermi$. By solving the Poisson equation with an assumed simple step-function distributions of the charge density in these two regions, the distribution of the electric field and the curvature radiation process of the accelerated particles can be calculated. In the our model, the properties of the phase-averaged spectrum can be completely specified by three gap parameters, i.e. the fractional gap size in the outer magnetosphere, the gap current in the primary region and the gap size ratio between the primary region and the total gap size. We discuss how these parameters affect the spectral properties. We argue that although the radiation mechanism in the outer gap is curvature radiation process, the observed gamma-ray spectrum can substantially deviate from the simple curvature spectrum because the overall spectrum consists of two components, i.e. the primary region and screening region. In some pulsars the radiation from the screening region is so strong that the photon index from 100MeV to several GeV can be as flat as $\sim 2$. We show the fitting fractional gap thickness of the canonical pulsars increases with the spin down age. We find that the total gap current is about 50~\% of the Goldreich-Julian value and the thickness of the screening region is a few percent of the total gap thickness. We also find that the predicted \gamma$-ray luminosity is less dependent on the spin down power ($L_{sd}$) for the pulsars with $L_{sd}\ga 10^{36}$~erg/s, while the $\gamma$-ray luminosity decreases with the spin down power for the pulsars with $L_{sd}\la 10^{36}$~erg/s.