Time-dependent escape of cosmic rays from supernova remnants potentially at the origin of the very-high-energy cosmic-ray gradient of the Galactic center

TL;DR

This paper investigates how the energy-dependent escape of cosmic rays from supernova remnants influences the gamma-ray emission morphology in the Galactic center, providing a better match to observations and predicting observable signatures for future telescopes.

Contribution

It introduces a time-energy dependent escape model for cosmic rays from supernova remnants, improving the explanation of the observed gamma-ray distribution in the Galactic center.

Findings

Energy-dependent escape shapes gamma-ray morphology.

Model aligns more closely with H.E.S.S. observations.

Predicts observable energy-dependent features for CTA.

Abstract

The distribution of the very-high-energy diffuse emission in the inner 200 pc measured by HE.S.S. indicates the existence of a pronounced cosmic-ray (CR) gradient peaking on the Galactic center (GC). Previous studies have shown that these data are consistent with a scenario in which the CRs are diffused away from a stationary source at the GC. We previously showed that, taking the 3D gas distribution and a realistic distribution of supernova explosions into account, CRs accelerated in supernova remnants (SNR) should account for a large fraction of the GC CRs observed by H.E.S.S.; but the model did not fully reproduce the apparent over-density in the inner 30 pc. In this work, we study the time-energy dependent cosmic rays escape from the remnant that is expected to occur when the shock wave decelerates in the surrounding medium. We show that the resulting CR distribution follows the quasi-stationary profile observed by H.E.S.S. more closely. The main signature is that the energy-dependent escape creates a strong dependency of the morphology of the gamma-ray emission with the energy. The existence of this energy dependency should be observable by the Cherenkov Telescope Array.