ICTS

In this lessons I will focus on the specificities of Extremely Precise Radial-Velocity (EPRV) Spectrographs and show on the basis of examples (HARPS, ESPRESSO and NIRPS) what makes the difference.

I will described how high-fidelity, radial-velocity spectrographs work and how they are employed for the search and characterisation of exoplanets

All magnetized solar system planets are strong radio emitters. Similar radio emissions have been found in the lowest mass stars and brown dwarfs and searches for radio emission from exoplanets is underway. These emissions are thought to be powered by various mechanisms drawing energy from the rotation of the emitting object, magnetic reconnection and/or magnetized wind impinging on the object. In this talk I will review the fundamentals of the relevant emission mechanisms, the plasma conditions that lead to such emissions, phenomenology of the observed emission and open questions in the field.

The observation of the first hot Jupiters around 3 decades ago has fuel the field of planet formation as the origin of these planets is still unknown at the present day. As such, planet formation models face the challenge to bridge two distinct states within the timeframe of the observations of planetary systems: the protoplanetary disc stage during which the planets form and the final (exo)-planetary system. This implies that models of planet formation need to include the structure and evolution of the protoplanetary discs, the accretion and migration processes of the growing planets as well as their composition. Consequently many different initial parameters of the disc (e.g. disc mass, disc radius, viscosity) and the planet (e.g. starting position and time) can be chosen. However, the number of observational constraints (e.g. planetary mass, final orbital distance) is limited, giving rise to a degeneracy within the models. A promising avenue to extend these observational constraints are measurements of atmospheric abundances, where observations via the JWST provide unprecedented data. In this talk, I will introduce the ingredients of planet formation models and how we can link these models to constraints from exoplanetary atmospheres to reveal the formation location of (hot) giant planets.

All magnetized solar system planets are strong radio emitters. Similar radio emissions have been found in the lowest mass stars and brown dwarfs and searches for radio emission from exoplanets is underway. These emissions are thought to be powered by various mechanisms drawing energy from the rotation of the emitting object, magnetic reconnection and/or magnetized wind impinging on the object. In this talk I will review the fundamentals of the relevant emission mechanisms, the plasma conditions that lead to such emissions, phenomenology of the observed emission and open questions in the field.

A pedagogical overview and tutorial on the current research in exoplanetary star planet magnetic interactions