The Mars Atmosphere and Volatile Evolution (MAVEN) Mission
The MAVEN spacecraft launched in November 2013, arrived at Mars in September 2014,
and completed commissioning and began its one-Earth-year primary science mission in …
and completed commissioning and began its one-Earth-year primary science mission in …
The analyzer of space plasmas and energetic atoms (ASPERA-3) for the Mars Express mission
The general scientific objective of the ASPERA-3 experiment is to study the solar wind–
atmosphere interaction and to characterize the plasma and neutral gas environment with …
atmosphere interaction and to characterize the plasma and neutral gas environment with …
Evolution of the solar activity over time and effects on planetary atmospheres. I. High-energy irradiances (1-1700 Å)
I Ribas, EF Guinan, M Güdel… - The Astrophysical …, 2005 - iopscience.iop.org
We report on the results of the Sun in Time multiwavelength program (X-rays to UV) of solar
analogs with ages covering∼ 0.1–7 Gyr. The chief science goals are to study the solar …
analogs with ages covering∼ 0.1–7 Gyr. The chief science goals are to study the solar …
Loss of the Martian atmosphere to space: Present-day loss rates determined from MAVEN observations and integrated loss through time
Observations of the Mars upper atmosphere made from the Mars Atmosphere and Volatile
Evolution (MAVEN) spacecraft have been used to determine the loss rates of gas from the …
Evolution (MAVEN) spacecraft have been used to determine the loss rates of gas from the …
How hospitable are space weather affected habitable zones? The role of ion escape
Atmospheres of exoplanets in the habitable zones around active young GKM stars are
subject to extreme X-ray and EUV (XUV) fluxes from their host stars that can initiate …
subject to extreme X-ray and EUV (XUV) fluxes from their host stars that can initiate …
Atmospheric loss of exoplanets resulting from stellar X-ray and extreme-ultraviolet heating
Past studies addressing the thermal atmospheric escape of hydrogen from" hot Jupiters"
have been based on the planet's effective temperature, which, as we show here, is not …
have been based on the planet's effective temperature, which, as we show here, is not …
Atmospheric escape processes and planetary atmospheric evolution
The habitability of the surface of any planet is determined by a complex evolution of its
interior, surface, and atmosphere. The electromagnetic and particle radiation of stars drive …
interior, surface, and atmosphere. The electromagnetic and particle radiation of stars drive …
Coronal mass ejection (CME) activity of low mass M stars as an important factor for the habitability of terrestrial exoplanets. II. CME-induced ion pick up of Earth-like …
Atmospheric erosion of CO2-rich Earth-size exoplanets due to coronal mass ejection (CME)-
induced ion pick up within close-in habitable zones of active M-type dwarf stars is …
induced ion pick up within close-in habitable zones of active M-type dwarf stars is …
The cosmic shoreline: The evidence that escape determines which planets have atmospheres, and what this may mean for Proxima Centauri B
KJ Zahnle, DC Catling - The Astrophysical Journal, 2017 - iopscience.iop.org
The Cosmic Shoreline: The Evidence that Escape Determines which Planets Have Atmospheres,
and what this May Mean for Proxima Centauri B - IOPscience This site uses cookies. By …
and what this May Mean for Proxima Centauri B - IOPscience This site uses cookies. By …
The evolution of solar flux from 0.1 nm to 160 μm: quantitative estimates for planetary studies
Understanding changes in the solar flux over geologic time is vital for understanding the
evolution of planetary atmospheres because it affects atmospheric escape and chemistry, as …
evolution of planetary atmospheres because it affects atmospheric escape and chemistry, as …