Cassini Reveals More About Cosmic Particle Accelerators

Shock waves are commonplace in the Universe, for example in the aftermath of a stellar explosion as debris accelerates outwards in a supernova remnant, or when the flow of particles from the Sun – the solar wind – impinges on the magnetic field of a planet to form a bow shock.

Under certain magnetic field orientations and depending on the strength of the shock, particles can be accelerated to close to the speed of light at these boundaries. Indeed, very strong shocks at young supernova remnants are known to boost electrons to ultra-relativistic energies, and may be the dominant source of cosmic rays, high-energy particles that pervade our Galaxy.


Space telescopes reveal evidence for accelerated electrons at supernova remnant shocks as X-ray emission, but these observations are made at great distances and thus the orientation of the local magnetic field can only be poorly measured at best. Without this crucial information, it is difficult to gain a full understanding of the shock acceleration process.

Scientists want to understand how the acceleration of electrons in very strong shocks with large ‘Mach numbers’ depends on the angle between the magnetic field and a vector at right angles to the shock front. In particular, they are interested in what happens in a ‘quasi-parallel’ shock, where the field and vector are almost aligned, as may be found in supernova remnants.

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source : www.esa.int