Coronal holes are the darkest and least active regions of the Sun, as observed both on the
solar disk and above the solar limb. Coronal holes are associated with rapidly expanding …

▪ Abstract Observational studies of low-mass stars during their early stages of evolution, from
protostars through the zero-age main sequence, show highly elevated levels of magnetic …

Photoionization heating from ultraviolet (UV) radiation incidents on the atmospheres of hot
Jupiters may drive planetary mass loss. Observations of stellar Lyman-α (Lyα) absorption …

We present a series of models for the plasma properties along open magnetic flux tubes
rooted in solar coronal holes, streamers, and active regions. These models represent the …

We present a comprehensive model of the global properties of Alfvén waves in the solar
atmosphere and the fast solar wind. Linear non-WKB wave transport equations are solved …

This chapter provides an overview of current efforts in the theory and modeling of CMEs.
Five key areas are discussed:(1) CME initiation;(2) CME evolution and propagation;(3) the …

The Sun, as an active star, is the driver of energetic phenomena that structure interplanetary
space and affect planetary atmospheres. The effects of Space Weather on Earth and the …

ABSTRACT A model is presented for generation of fast solar wind in coronal holes, relying
on heating that is dominated by turbulent dissipation of MHD fluctuations transported …

Using empirical ion velocity distributions derived from Ultraviolet Coronagraph Spectrometer
(UVCS) and Solar Ultraviolet Measurements of Emitted Radiation (SUMER) ultraviolet …

Coronal holes are the lowest density plasma components of the Sun's outer atmosphere,
and are associated with rapidly expanding magnetic fields and the acceleration of the high …