Measuring the cosmic ray acceleration efficiency of a supernova remnant

TL;DR

This study demonstrates that cosmic rays significantly contribute to the pressure behind a supernova remnant shock, indicating a high acceleration efficiency, by combining optical spectroscopy and X-ray observations.

Contribution

It provides the first direct measurement of cosmic-ray pressure contribution in a supernova remnant using combined optical and X-ray data.

Findings

Cosmic-ray pressure exceeds thermal pressure behind the shock.

More than 50% of post-shock pressure is due to cosmic rays.

Standard shock heating models do not match observed proton temperatures.

Abstract

Cosmic rays are the most energetic particles arriving at earth. Although most of them are thought to be accelerated by supernova remnants, the details of the acceleration process and its efficiency are not well determined. Here we show that the pressure induced by cosmic rays exceeds the thermal pressure behind the northeast shock of the supernova remnant RCW 86, where the X-ray emission is dominated by synchrotron radiation from ultra-relativistic electrons. We determined the cosmic-ray content from the thermal Doppler broadening measured with optical spectroscopy, combined with a proper-motion study in X- rays. The measured post-shock proton temperature in combination with the shock velocity does not agree with standard shock heating, implying that >50% of the post-shock pressure is produced by cosmic rays.