EUV influences on exoplanet atmospheric stability and evolution. (arXiv:1903.05718v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Youngblood_A/0/1/0/all/0/1">Allison Youngblood</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+France_K/0/1/0/all/0/1">Kevin France</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koskinen_T/0/1/0/all/0/1">Tommi Koskinen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fossati_L/0/1/0/all/0/1">Luca Fossati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amerstorfer_U/0/1/0/all/0/1">Ute Amerstorfer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lichtenegger_H/0/1/0/all/0/1">Herbert Lichtenegger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drake_J/0/1/0/all/0/1">Jeremy Drake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mason_J/0/1/0/all/0/1">James Mason</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fleming_B/0/1/0/all/0/1">Brian Fleming</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allred_J/0/1/0/all/0/1">Joel Allred</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berta_Thompson_Z/0/1/0/all/0/1">Zachory Berta-Thompson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bourrier_V/0/1/0/all/0/1">Vincent Bourrier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Froning_C/0/1/0/all/0/1">Cynthia Froning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garraffo_C/0/1/0/all/0/1">Cecilia Garraffo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gronoff_G/0/1/0/all/0/1">Guillaume Gronoff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jin_M/0/1/0/all/0/1">Meng Jin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kowalski_A/0/1/0/all/0/1">Adam Kowalski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Osten_R/0/1/0/all/0/1">Rachel Osten</a>
The planetary effective surface temperature alone is insufficient to
characterize exoplanet atmospheres and their stability or evolution.
Considering the star-planet system as a whole is necessary, and a critical
component of the system is the photoionizing stellar extreme ultraviolet
emission (EUV; 100-912 {AA}). EUV photons drive atmospheric mass loss through
thermal and nonthermal processes, and an accurate accounting of the EUV energy
deposition in a planet’s energy budget is essential, especially for terrestrial
habitable zone planets and close-in gaseous planets. Direct EUV observations of
exoplanet host stars would require a new, dedicated observatory. Archival
observations from the $textit{EUVE}$ satellite, models, and theory alone are
insufficient to accurately characterize EUV spectra of the majority of
exoplanet host stars, especially for low-mass stars.
The planetary effective surface temperature alone is insufficient to
characterize exoplanet atmospheres and their stability or evolution.
Considering the star-planet system as a whole is necessary, and a critical
component of the system is the photoionizing stellar extreme ultraviolet
emission (EUV; 100-912 {AA}). EUV photons drive atmospheric mass loss through
thermal and nonthermal processes, and an accurate accounting of the EUV energy
deposition in a planet’s energy budget is essential, especially for terrestrial
habitable zone planets and close-in gaseous planets. Direct EUV observations of
exoplanet host stars would require a new, dedicated observatory. Archival
observations from the $textit{EUVE}$ satellite, models, and theory alone are
insufficient to accurately characterize EUV spectra of the majority of
exoplanet host stars, especially for low-mass stars.
http://arxiv.org/icons/sfx.gif
