Results 21 to 30 of about 221 (127)
HUBBLE SPACE TELESCOPE CONSTRAINTS ON THE WINDS AND ASTROSPHERES OF RED GIANT STARS* [PDF]
The Astrophysical Journal, 2016 ABSTRACT We report on an ultraviolet spectroscopic survey of red giants observed by the Hubble Space Telescope, focusing on spectra of the Mg ii h and k lines near 2800 Å in order to study stellar chromospheric emission, winds, and astrospheric absorption.
Brian E. Wood +2 more
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MHD equilibria of astrospheric flows [PDF]
, 2005 The hot gas cavities around stars which have a stellar wind are called astrospheres. Between the outer interstellar medium and the stellar wind there forms a contact surface or boundary surface which is called an astropause. In this thesis the geometrical shape of such an astrosphere/astropause region is calculated consistently together with the flow ...
Nickeler, Dieter Horst
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Astrospheric evolution and cosmic-ray particle transport [PDF]
Doctor of Philosophy Science with Physics, North-West University, Potchefstroom ...
Light, Juandre
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On the problem of two-tail heliosphere/astrospheres
Journal of Physics: Conference Series, 2018 Vladislav Izmodenov, Dmitry Alexashov
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Solar wind with Hydrogen Ion charge Exchange and Large-Scale Dynamics (SHIELD) DRIVE Science Center
Frontiers in Astronomy and Space Sciences, 2023 Most stars generate winds and move through the interstellar medium that surrounds them. This movement creates a cocoon formed by the deflection of these winds that envelops and protects the stars. We call these “cocoons” astrospheres. The Sun has its own
Merav Opher +48 more
doaj +1 more source
Astrospheres of planet-hosting cool stars and beyond when modeling meets observations [PDF]
, 2022 Thanks to dedicated long-term missions like Voyager and GOES over the past 50 years, much insight has been gained on the activity of our Sun, the solar wind, its interaction with the interstellar medium, and, thus, about the formation, the evolution, and
Herbst, Konstantin Linus +13 more
core +1 more source
The Kelvin-Helmholtz instability in astrospheres.
, 2022 Videos are isolines of the Mach number in the entire flow area versus time. You can observe the evolution of the Kelvin-Helmholtz instability. Video_1 shows the flow with the parameter \(\chi = 1.6\) and \(M_\infty = 3\). It's almost a steady stream. Video_2 shows the flow with the parameter \(\chi = 17\) and \(M_\infty = 3\).
Korolkov, S.D., Izmodenov, V.V.
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Modeling the astrosphere of LHS~1140 [PDF]
Astronomy & Astrophysics14 pages, 8 ...
Scherer, K. +5 more
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Astrospheres, stellar winds, and the interstellar medium
, 2016 Brian E. Wood, Jeffrey L. Linsky
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Journal of Geophysical Research: Space Physics, Volume 124, Issue 12, Page 9774-9790, December 2019., 2019 Abstract Computation of the ionization and radiation dose in arbitrary (exo‐) planetary atmospheres due to energetic particles is recently becoming more important due to several reasons that are either correlated with the detection of trace gases for life on exoplanets or with computing dose rates at arbitrary altitudes in the Earth atmosphere.
S. Banjac +4 more
wiley +1 more source