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New Mass-Loss Measurements from Astrospheric Lyα Absorption
Measurements of stellar mass-loss rates are used to assess how wind strength varies with coronal activity and age for solar-like stars. Mass loss generally increases with activity, but we find
Measured Mass‐Loss Rates of Solar‐like Stars as a Function of Age and Activity
Collisions between the winds of solar-like stars and the local interstellar medium result in a population of hot hydrogen gas surrounding these stars. Absorption from this hot H i can be detected in
Stellar Lyα Emission Lines in the Hubble Space Telescope Archive: Intrinsic Line Fluxes and Absorption from the Heliosphere and Astrospheres*
We search the Hubble Space Telescope (HST) archive for previously unanalyzed observations of stellar H I Lyα emission lines, our primary purpose being to look for new detections of Lyα absorption
A nonlinear theory of the perpendicular diffusion of charged particles is presented, including the influence of parallel scattering and dynamical turbulence. The theory shows encouraging agreement
The Heliosphere’s Interstellar Interaction: No Bow Shock
Combined consensus values for this velocity vector are provided and show that they have important implications for the global interstellar interaction, in particular, the velocity is almost certainly slower than the fast magnetosonic speed, with no bow shock forming ahead of the heliosphere, as was widely expected in the past.
Interaction of the solar wind with the local interstellar medium: a theoretical perspective
The interaction of the solar wind with the local interstellar medium (LISM) is attracting renewed interest, thanks to the possibility that the Voyager spacecraft may, in the not too distant future,
Mechanisms for the deposition of heat in the lower coronal plasma are discussed, emphasizing recent attempts to reconcile the —uid and kinetic perspectives. Structures at magnetohydrodynamic (MHD)
Dust in the local interstellar wind
The gas-to-dust mass ratios found for interstellar dust within the solar system, versus values determined astronomically for the cloud around the solar system, suggest that large and small
Coronal Heating by Magnetohydrodynamic Turbulence Driven by Reflected Low-Frequency Waves
A candidate mechanism for the heating of the solar corona in open field line regions is described. The interaction of Alfven waves, generated in the photosphere or chromosphere, with their
Coronal Heating Distribution Due to Low-Frequency, Wave-driven Turbulence
The heating of the lower solar corona is examined using numerical simulations and theoretical models of magnetohydrodynamic turbulence in open magnetic regions. A turbulent energy cascade to small