Тип публикации: статья из журнала

Год издания: 2022

Идентификатор DOI: 10.1007/s11214-022-00876-5

Ключевые слова: dust, mercury, moon, planetary embryos, rocky close-in exoplanets, young sun

Аннотация: In this review we discuss all the relevant solar/stellar radiation and plasma parameters and processes that act together in the formation and modification of atmospheres and exospheres that consist of surface-related minerals. Magma ocean degassed silicate atmospheres or thin gaseous envelopes from planetary building blocks, airlesПоказать полностьюs bodies in the inner Solar System, and close-in magmatic rocky exoplanets such as CoRot-7b, HD 219134 b and 55 Cnc e are addressed. The depletion and fractionation of elements from planetary embryos, which act as the building blocks for proto-planets are also discussed. In this context the formation processes of the Moon and Mercury are briefly reviewed. The Lunar surface modification since its origin by micrometeoroids, plasma sputtering, plasma impingement as well as chemical surface alteration and the search of particles from the early Earth’s atmosphere that were collected by the Moon on its surface are also discussed. Finally, we address important questions on what can be learned from the study of Mercury’s environment and its solar wind interaction by MESSENGER and BepiColombo in comparison with the expected observations at exo-Mercurys by future space-observatories such as the JWST or ARIEL and ground-based telescopes and instruments like SPHERE and ESPRESSO on the VLT, and vice versa. © 2022, The Author(s).

Журнал: Space Science Reviews

Выпуск журнала: Vol. 218, Is. 3

Номера страниц: 15

ISSN журнала: 00386308

Издатель: Springer Science and Business Media B.V.

• Lammer H. (Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, Graz, 8042, Austria)
• Scherf M. (Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, Graz, 8042, Austria, Institute of Physics/IGAM, University of Graz, Graz, Austria, Institute of Geodesy, Technical University of Graz, Graz, Austria)
• Ito Y. (Dept. of Physics and Astronomy, Faculty of Maths and Physical Sciences, University College London, Gower Street, London, WC1E 6BT, United Kingdom, National Astronomical Observatory of Japan, Osawa 2-21-1, Tokyo, Mitaka, 181-8588, Japan)
• Mura A. (Istituto de Fisica dello Spazio Interplanetario-CNR, Rome, Italy)
• Vorburger A. (Physikalisches Institut, University of Bern, Bern, Switzerland)
• Guenther E. (Thüringer Landessternwarte Tautenburg – Karl-Schwarzschild-Observatorium, Sternwarte 5, Tautenburg, 07778, Germany)
• Wurz P. (Physikalisches Institut, University of Bern, Bern, Switzerland)
• Erkaev N.V. (Institute of Computational Modelling, Siberian Branch of the Russian Academy of Sciences, Krasnoyarsk, 660036, Russian Federation, The Applied Mechanics Department, Siberian Federal University, Krasnoyarsk, 660074, Russian Federation, Institute of Laser Physics, Siberian Branch of the Russian Academy of Sciences, Novosibirsk, 630090, Russian Federation)
• Odert P. (Institute of Physics/IGAM, University of Graz, Graz, Austria)

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