Host Stars and their Effects on Exoplanet Atmospheres by Jeffrey Linsky

Author:Jeffrey Linsky
Language: eng
Format: epub
ISBN: 9783030114527
Publisher: Springer International Publishing

Included in Table 8.2 are simulations of stellar winds and the solar wind at different ages (100 Myr and 700 My) and various conditions (for minimum and maximum activity today, X-ray surface flux F x = 106 erg cm−2 s−1, and for saturated mass-loss rate). These simulations assume that the thermal distribution where the winds are driven is either computed from the dissipation of Alfvén waves or approximated through the value of the assumed polytrope index α. There are systematic errors associated with both types of models. Both types must assume a value for the density at the base of the wind and are based upon observed magnetic field images with low spatial resolution. The Alfvén wave driven simulations assume a specific type of magnetic wave, whereas there are a variety of such waves and energy conversion among these waves. The polytropic simulations assume a coronal temperature based on solar analogy, but depends sensitively on the coronal temperature (cf., Airapetian and Usmanov 2016). The orbital speeds of close-in Jupiters are supermagnetosonic with bow shocks surrounding the exoplanets as they plow through the stellar wind (Vidotto et al. 2015).Table 8.2MHD simulations of winds based on magnetic images

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