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It is currently unknown how common life is on exoplanets, or how long planetscan remain viable for life. To date, we have a superficial notion ofhabitability, a necessary first step, but so far lacking an understanding ofthe detailed interaction between stars and planets over geological timescales,dynamical evolution of planetary systems, and atmospheric evolution on planetsin other systems. A planet mass, net insolation, and atmospheric compositionalone are insufficient to determine the probability that life on a planet couldarise or be detected. The latter set of planetary considerations, among others,underpin the concept of the habitable zone (HZ), defined as the circumstellarregion where standing bodies of liquid water could be supported on the surfaceof a rocky planet. However, stars within the same spectral class are oftentreated in the same way in HZ studies, without any regard for variations inactivity among individual stars. Such formulations ignore differences in hownonthermal emission and magnetic energy of transient events in different starsaffect the ability of an exoplanet to retain its atmosphere.In the last fewyears there has been a growing appreciation that the atmospheric chemistry, andeven retention of an atmosphere in many cases, depends critically on thehigh-energy radiation and particle environments around these stars. Indeed,recent studies have shown stellar activity and the extreme space weather, suchas that created by the frequent flares and coronal mass ejections (CMEs) fromthe active stars and young Sun, may have profoundly affected the chemistry andclimate and thus habitability of the early Earth and terrestrial typeexoplanets. The goal of this white paper is to identify and describe promisingkey research goals to aid the field of the exoplanetary habitability for thenext 20 years.

Exploring Extreme Space Weather Factors of Exoplanetary Habitability