Magnetospheres of neutron stars (NSs) represent unique plasma-physics labs of extreme environments characterized by ultra-high magnetic field strengths, relativistic processes, and the presence of quantum electrodynamic effects – parameters far unreachable on the Earth. Detailed information on these processes comes to us via coherent radio emissions of pulsars and possibly fast radio bursts (FRBs), being observed by fast-developing sophisticated instruments of radio astronomy like FAST, CHIME, ALMA, and in near future, SKA. However, no agreement has been reached on their exact coherent radio emission mechanism that can interpret the observations, mainly because the modeling of the radio emissions requires operation of the extreme-physical processes and simultaneous consideration of the wave coherency at plasma kinetic micro-scales. This project addresses the question of which specific mechanisms are responsible for coherent radio emissions of NSs; in detail, which qualitative radio emission properties of pulsar pair-creation events and propagating kinetic Alfvén waves in the magnetospheres of NSs can lead to the interpretation of pulsars and transient events like fast radio bursts. The mechanisms will be investigated by combination of my expertise in first-principle particle-in-cell simulations of the micro-kinetic instabilities with the long-term experience in advanced dispersion and coherency analyses of radio waves in the simulations at the host institute. This combination of skills will allow me to make predictions on coherent properties of radio waves in terms of their total power, luminosity spectrum, its directivity and polarization as they escape the emission sources. I will distinguish, for the first time, how the extreme plasma instabilities lead to the coherent and incoherent radio emissions of pulsars and FRBs. After the project, the obtained properties can be utilized in radiative transfer codes to get specific predictions on NS radio observables.

Massive stars are the cornerstone of the dynamic and chemical evolution of the cosmos, enriching it as they evolve with chemically processed material that is blown away from their surface by energetic winds and eruption processes. Despite their importance, their evolution from cradle to death as spectacular supernova explosions still poses many mysteries due to crucial knowledge gaps in the physical processes taking place in their interior and atmosphere and the mutual influence by close-by siblings. Our ultimate goal is to elucidate the physical properties and evolution of massive stars impacted by companions, as well as their contribution to the generation of gravitational waves. For this, we wish to establish a multidisciplinary, international network of researchers from Europe and America with expertise in various disciplines, and with background in both theory and observations. We will exploit the avalanche of public data archives and develop machine learning algorithms to detect massive stars in binary and multiple systems, classify them, and create statistically meaningful samples for diverse evolutionary states. We will develop progressive methods of signal processing for the analysis of the stellar properties, and cutting-edge numerical codes to unveil the impact of stellar interaction and mass ejection on the evolution of the stars and stellar systems. The acquired results will significantly enhance our knowledge and lead to major advancements in all related fields. The bulk of exchanges will be undertaken by PhD students and Postdocs, whom we will educate and train in modern observing and data analysing techniques, machine learning algorithms, and in high-performance computing, equipping them with excellent skills for their future careers. We will organise schools, workshops and educational activities to share knowledge as well as disseminate our results, which will be major breakthroughs and will expand Europe's leading role in basic research.

Massive stars are extreme cosmic engines, enriching their environments with chemically processed material throughout their entire life-time, and triggering star and planet formation. Despite their importance for the cosmic evolution, their evolutionary path up to their deaths as spectacular supernova explosions is most uncertain due to the lack of precise knowledge of the physical mechanisms behind mass eruptions. We wish to establish a multidisciplinary, international network of researchers from Europe, Asia, and South America with expertise in a variety of disciplines, and with background in both theory and observations. Our ultimate goal is to enlighten the processes that trigger mass loss in massive stars during extreme phases of their evolution. We will develop cutting-edge numerical codes suitable to describe the chemical and dynamical evolution of the stars, their winds, and their large-scale environments. In addition, we will initiate global observing campaigns utilizing facilities at major renowned observatories in combination with our national facilities, and exploit public archives from ground-based and space missions to acquire an outstanding set of urgently needed highest quality data. Confronting predictions from the numerical models with the observations will empower us to derive the first extensive and comprehensive set of precise physical parameters. The acquired results will significantly enhance our knowledge and lead to major advancements in all related fields. The bulk of exchanges will be undertaken by Early Stage Researchers and young Post-docs, who will be educated and trained in modern observing and data analyzing techniques and in high-performance computation, equipping them with excellent skills for their future careers. We will organize schools and workshops to share knowledge and to communicate and disseminate our results, which will be major breakthroughs and support the leading role of Europe in Astronomy.