Titlebook: Host Stars and their Effects on Exoplanet Atmospheres; An Introductory Over Jeffrey Linsky Book 20191st edition Springer Nature Switzerland

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Stellar Chromospheres: The Source of UV Emission,vection heat from below and the loss of radiation to space. With increasing height in a stellar atmosphere, magnetic heating processes become important in the energy balance, forcing the temperature to increase with height in a region called the chromosphere. Magnetic heating processes include the d

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Stellar Coronae: The Source of X-ray Emission, space. However, the hottest region of a star can be its outermost layer, the corona with temperatures of 10. K to 10. K or even hotter. The heating mechanism responsible for hot coronae has been debated since the existence of hot coronal gas was first identified in the early 1940s.

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Stellar Winds,r layers of exoplanet atmospheres producing charge-exchange and other reactions that facilitate mass loss. In this chapter, I describe the different types of winds observed in hot and cool stars. For some star types, it is relatively easy to measure diagnostics of mass loss but in solar type stars i

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Host Star Driven Exoplanet Mass Loss and Possible Surface Water,planet atmospheres. The main thermal process is hydrodynamical outflow driven by extreme ultraviolet and x-radiation from the host star that heat and inflate an exoplanet’s exosphere leading to mass loss. Non-thermal mass loss occurs when ions and electrons in the host star’s wind remove neutrals an

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Space Weather: The Effects of Host Star Flares on Exoplanets,s usually benign, exoplanets located close to their host stars, especially active M dwarfs, must suffer through powerful flares, stellar winds, CMEs, and very high energy radiation. The environment in which exoplanets must live is now called “stellar space weather” in analogy with the extensively mo

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