How are magnetic fields amplified, and how do they evolve and affect the dynamics and properties of the ionized media?
What physical mechanisms drive the transport and acceleration of cosmic rays in diverse plasma environments, and how do they shape the overall energy budget?
Can current theoretical models explain the relativistic plasma structures that are being observed?
What are testable predictions for probing the fundamental properties of non-thermal and thermal plasma phenomena linking micro to macro-scale processes?
How does the population of cosmic rays evolve and accelerate in magnetized radio filaments in different environments?
Cosmic Ray Transport and Acceleration
Cosmic Magnetic Fields in Diverse Environments
Micro and Macro Plasma Processes
Andra Stroe (CfA/STScI) Alexander A. Schekochihin (University of Oxford)
Christine Jones (CfA) Andra Stroe (CfA/Space Telescope Science Institute)
Ewan O'Sullivan (CfA) Andrea Botteon (INAF- Istituto di Radioastronomia)
Gerrit Schellenberger (CfA) Christoph Pfrommer (University of Potsdam)
Jaya Maithil (CfA, co-chair) Eugene Churazov (Max Planck Institute for Astrophysics)
Jan Vrtilek (CfA) Ewan O'Sullivan (CfA)
Kamlesh Rajpurohit (CfA, chair) Kamlesh Rajpurohit (CfA-chair)
Laurence David (CfA) Marcus Brüggen (University of Hamburg)
Paola Domínguez Fernández (CfA) Marisa Brienza (INAF- Istituto di Radioastronomia)
Romeo Giancarlo (CfA) Matthias Hoeft (Thüringer Landessternwarte Tautenburg)
Tirna Deb (CfA) Paola Domínguez Fernández (CfA)
William Forman (CfA) William Forman (CfA, co-chair)