Due to their large number within the Galaxy, their small radii, and closer-in habitable zones (HZ), G-, K- and M-dwarf stars are prime targets for detecting habitable rocky (Earth-like) exoplanets. Next generation missions such as JWST, ARIEL, the ELT and LIFE could in principle detect atmospheric biosignatures (indicators for life) in exoplanetary atmospheres of planets orbiting distant stars. It is therefore timely for theoretical background studies focusing on the particle- and radiation environment of Earth-like exoplanets in the HZ of G-, K-, and M-dwarf stars and their imprint on planetary habitability. Although the presence of liquid water on the surface of such worlds is a key requirement for life as we know it, it is likely not the only criterium. The presence of strong stellar winds, which can lead to the erosion of unprotected planetary atmospheres, and/or extreme stellar particle events as well as coronal mass ejections which induce changes in the atmospheric composition via photochemical effects as well as changes in the atmospheric secondary particle environment. Such effects may destroy atmospheric biosignatures and could prevent the creation and development of life. Thus, detailed knowledge of the astrosphere as well as the astrospheric particle- and radiation environment is mandatory in order to study planetary habitability. Now is the time to make use of what we have learnt from the Sun and our solar system to extend our knowledge to extrasolar planetary systems with potentially Earth-like exoplanets in the HZs of G-, K- and M-dwarf stars.

The session brings together scientists from all fields of research that are related to solar, astrophysical, and exoplanetary sciences. It will allow the sharing of expertise amongst researchers working on different aspects of this interdisciplinary scientific field, allowing showcases of recent advancements in the field of specialization. The session aims to stimulate discussions on how individual disciplines can share their knowledge and benefit from each other.

We solicit contributions related but not limited to:

• Modeling stellar astrospheres and the corresponding energy-dependent CR flux
• Modeling the environment of close-in exoplanets around G-, K-, and M-dwarf stars, in particular, modeling of mass-loss rates, angular momentum loss rates, the magnetic field configuration as well as the density and velocity of the stellar winds of G-, K- and M-dwarf stars
• Modeling stellar CMEs
• Evaluation and quantification of the solar UV-, X-ray, and energetic particle flux relationships and their extension to G-, K-, and M-dwarf stars
• The imprint of the stellar radiation field by modeling the magnetospheric transport and particle interactions within (exo)planetary atmospheres
• Atmospheric modeling studies of climate and (biosignature) photochemistry and the influence of stellar activity

Public Comment:

The session brings together scientists from all fields of research that are related to solar- and astrophysical sciences. We aim to stimulate discussions about how individual disciplines can share their knowledge and benefit from each other.