Atmospheric and water loss from early Venus

By Y. Kulikov, H. Lammer, H. Lichtenegger, N. Terada, I. Ribas, C. Kolb, D. Langmayr, R. Lundin, E. Guinan, S. Barabash and 1 more. 2006

135 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/2e64118e4294ccab2319622ef24c4d68d14fe1aa

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Aerospace Engineering

1. R. Roble
2. F. Tian
3. Han-Li Liu
4. J. Kasting

In Astronomy and Astrophysics

1. M. Gudel
2. R. Nakamura
3. Han-Li Liu
4. Wolfgang Baumjohann
5. H. Lammer
6. J. Kasting
7. A. Balogh
8. F. Tian

Citations in the corpus

• The Sun in Time: Activity and Environment (2007, methodology): “The only independent variable, the stellar age, then determines the rotation period and, through the internal magnetic dynamo, magnetic activity at all levels of the stellar atmosphere, probably including characteristics of the stellar wind (Wood et al., 2002, 2005; Kulikov et al., 2006).”
• WATER LOSS FROM TERRESTRIAL PLANETS WITH CO2-RICH ATMOSPHERES (2013, unknown): “Finally, CO 2 can also directly limit the escape of hydrogen in the highest part of the atmosphere, because its effectiveness as an emitter of thermal radiation in the IR means it can “scavenge” energy that would otherwise be used to power hydrogen escape (Kulikov et al. 2006; Tian et al. 2009).”
• Magnetic field investigation of the Venus plasma environment: Expected new results from Venus Express (2006, background): “…observations will allow us, to get a better understanding of contribution of the loss due to ion clouds compared to ion pick up over the whole solar activity cycle, which is important for models, which are applied to the study of evolutionary aspects of Venus’ atmosphere (see Kulikov et al., 2006).”
• Hydrodynamic planetary thermosphere model: 1. Response of the Earth's thermosphere to extreme solar EUV conditions and the significance of adiabatic cooling (2008, background): “For EUV fluxes greater than 5 present EUV, hydrodynamic flow and adiabatic cooling take place so that the Kulikov et al. model is no longer valid. Despite the difference in finding the exobase under extreme solar EUV fluxes, the fact that extremely high exobase temperatures are given by Kulikov et a”
• Atmospheric Escape and Evolution of Terrestrial Planets and Satellites (2008, methodology): “Additionally, the soft X-rays and EUV radiation is absorbed in a planetary thermosphere, whereby it can heat and expand it significantly (e.g., Lammer et al. 2006a, 2007; Kulikov et al. 2006, 2007; Tian et al. 2008).”