Selected Student Papers

A large-scale magnetic field (ranging from a fraction of a μG to hundreds of mG) permeates the interstellar medium (ISM) of our Galaxy and is involved in a variety of astrophysical properties (e.g. star formation, cosmic ray propagation). Characterizing the magnetic field properties is necessary in order to understand these processes. Dust polarization has been proven one of the most powerful observables for studying the field properties in the ISM, although it probes only the magnetic field orientation and not its strength. For this reason, various methods which infer the magnetic field strength have been developed. The most widely applied method has been developed by Davis (1951) and Chandrasekhar & Fermi (1953) (DCF). This method relies on the assumption that the observed spread in the distribution of polarization angles is due to the propagation of the so-called Alfvén magnetohydrodynamic waves. Observations, however, indicate that non-Alfvénic (compressible) modes may be important in the ISM dynamics. In this work we propose a new method for estimating the magnetic field strength which includes the compressible modes. We have tested our method in MHD numerical simulations and we compared it with the classical DCF method. In the figure to the left it is shown that our method outperforms the previous methods, which are based solely on Alfvénic modes, and achieves a mean relative deviation of 17% without the need for a correction.

Research Articile: “High-accuracy estimation of magnetic field strength in the interstellar medium from dust polarization”, R. Skalidis, K. Tassis,  2021, A&A, 647, 186 – March 2021