X‐exoplanets coronal models and planet photoevaporation

Abstract: High‐energy emission photons in the X‐ray and EUV bands ionize H and other atoms, posing a threat to the stability of the atmospheres of short‐period exoplanets orbiting late‐type stars. Effects such as planet atmospheric evaporation are being attributed in the last years to XUV stellar irradiation on the planets. Early theoretical works tried to model how the XUV emission would affect the planetary atmospheres, mainly by using the solar emission as a template. In X‐exoplanets, we reported for the first time coronal models based on actual data from the exoplanet host stars. The use of coronal models allows us to model the SED of the XUV emission of these stars, otherwise inaccessible to current telescopes. In this manuscript, I present the use of these models with datasets of different data quality, depending on the availability of low or high spectral resolution spectra in both X‐rays and UV. Comparison with actual data is shown for the exoplanet host star Proxima Cen and the Sun. The challenges for the future use of coronal models in exoplanet atmospheres are discussed, involving mainly the use of new EUV and X‐ray spectrographs, better atomic models, and more accurate planet atmosphere evolution models.

Show object

• Location: Deutsche Nationalbibliothek Frankfurt am Main
• Extent: Online-Ressource
• Language: Englisch

References and Relationships

• Bibliographic citation: X‐exoplanets coronal models and planet photoevaporation ; day:01 ; month:02 ; year:2022 ; extent:6 ; Astronomische Nachrichten ; (01.02.2022) (gesamt 6)

Contributors, Places and Time

• Creator: Sanz‐Forcada, Jorge

Further information

• DOI: 10.1002/asna.20220008
• URN: urn:nbn:de:101:1-2022020214003938439632
• Rights: Open Access; Der Zugriff auf das Objekt ist unbeschränkt möglich.