How has the solar wind evolved to reach what it is today? In this review, I discuss the long-
term evolution of the solar wind, including the evolution of observed properties that are …

We present results from a set of numerical simulations aimed at exploring the mechanism of
coronal mass ejection (CME) suppression in active stars by an overlying large-scale …

We consider the physical characteristics and dynamics of the gaseous envelopes of hot
Jupiters (HJs)—gas giants with a mass comparable to Jupiter's and a semi-major axis of less …

Solar coronal mass ejections (CMEs) and flares have a statistically well-defined relationship,
with more energetic X-ray flares corresponding to faster and more massive CMEs. How this …

The atmospheres of highly irradiated exoplanets are observed to undergo hydrodynamic
escape. However, due to strong pressures, stellar winds can confine planetary atmospheres …

High-energy stellar irradiation can photoevaporate planetary atmospheres, which can be
observed in spectroscopic transits of hydrogen lines. For the exoplanet HD189733b …

The M dwarf star GJ 436 hosts a warm-Neptune that is losing a substantial amount of
atmosphere, which is shaped by the interactions with the wind of the host star. The stellar …

The Extreme-ultraviolet Stellar Characterization for Atmospheric Physics and Evolution
(ESCAPE) mission is an astrophysics Small Explorer employing ultraviolet spectroscopy …

Coronal mass ejections (CMEs) on stars other than the Sun have proven very difficult to
detect. One promising pathway lies in the detection of type II radio bursts. Their appearance …

As a rule, the orbits of “hot Jupiter” exoplanets are located close to the Alfven point of the
stellar wind of the host star. Many hot Jupiters could be in the sub-Alfven zone, where the …