MHD Modes in the ISM: A Statistical Approach Using Synchrotron Polarization

by Parth Pavaskar (University of Potsdam & DESY Zeuthen)

Wednesday May 13, 2026, 3:00 PM → Friday May 15, 2026, 4:30 PM Europe/Madrid

00.303.0 - Aula 13 (Facultad de Ciencias Físicas)

Magnetohydrodynamic (MHD) turbulence plays a fundamental role in shaping the interstellar medium (ISM), influencing cosmic ray transport, star formation, and plasma dynamics. The properties of the MHD turbulence are governed by the energy fractions of the three fundamental plasma modes: the incompressible Alfvén, and the compressible fast and slow modes. However, identifying which mode dominates the energy remains a significant observational challenge. I will present the modified Synchrotron Polarization Analysis (SPA+) method, a technique to systematically identify the dominant MHD mode in ISM plasma using synchrotron polarization observations, helping us model the aforementioned processes better. I will further show the application of this method to real observations, analyzing the magnetized turbulence in the Cygnus loop region.

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