Notes on non-thermal X-ray radiation of radio supernova remnant W50 and collimated radiation of SS433

TL;DR

This paper investigates non-thermal X-ray emission from the W50 nebula and SS433 jets, proposing a collimated inverse-Compton scattering model to address synchrotron model issues, with implications for particle energies and observational sensitivity.

Contribution

It introduces a collimated inverse-Compton scattering model for W50 and SS433 X-ray emission, offering an alternative to synchrotron models and analyzing energy constraints and observational detectability.

Findings

Inapplicability of the model at minimal Lorentz factors due to excessive particle energy.

At higher Lorentz factors, the emission shifts outside the 1-10 keV observational band.

Existing data are insensitive to the emission cone at Lorentz factors greater than 10.

Abstract

Diffuse X-ray emission of the radio nebula W50 along the line of the of jets of the microquasar SS433 has a non-thermal power law component. This could be the inverse-Compton scattered emission of the SS433 accretion disk funnel, which is collimated in a cone before the scattering off relativistic electrons - so called emission cone, hypothetical and invisible directly. This model would remove the synchrotron model problems of the X-ray emission: of acceleration of the emitting electrons to extreme Lorenz factors $\gamma > 10^9$ in the mildly relativistic SS433 jets and morphological difference of W50 in the synchrotron radio and X-ray bands. Our study of the comptonization model showed up that in the case of the minimal factor $\gamma_{\rm min}$ of the order 1 the energy of the relativistic particles, which upscatter the cone photons, is close to or exceeds total energy of the nebula - the case of inapplicability of the model. In the case of $\gamma_{\rm min} > 10$ the cone emission is comptonized beyond the 1 - 10\,keV band, consequently the existing observational data are non-sensitive to the emission cone.