Conclusion

Chapter
Part of the SpringerBriefs in Astronomy book series (BRIEFSASTRON)

Abstract

The atmosphere evolution of terrestrial planets from the origin of protoatmospheres throughout the most active period of a planet’s host star until the star’s activity decreased to moderate and quiet levels is discussed. The first protoatmosphere will be captured and accumulated hydrogen- and helium-rich gas envelopes from the nebula. Depending on the planetary formation time, the nebula dissipation time, the numbers of additional planets including gas giants in the system, the protoplanet’s gravity, its orbit location, and the host star’s radiation and plasma environment terrestrial planets may capture tens or even several hundreds of the Earth ocean equivalent amounts of hydrogen around its rocky core.

Keywords

Solar Wind Terrestrial Planet Host Star Rocky Core Atmosphere Evolution 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Copyright information

© The Author(s) 2013

Authors and Affiliations

  1. 1.Space Research InstituteAustrian Academy of SciencesGrazAustria

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