|
Turbulence and magnetic fields are both ubiquitous in the Milky Way, significantly affecting the formation of stars, and how gas is recycled in the Galaxy. However, the nature of turbulent flows in the magnetised interstellar medium is largely unknown, as key properties of turbulence are poorly constrained by observations. I will discuss how observations of synchrotron intensity fluctuations can be used to probe the sonic and Alfvenic Mach numbers of interstellar turbulence, based on mock observations performed on simulations of magneto-hydrodynamic turbulence. I will also discuss the potential for novel polarisation analysis techniques to uniquely determine the sonic and Alfvenic Mach numbers of observed turbulence, and to assist in qualitative understanding of Galactic magneto-ionic turbulence. |
|