Studies in the Future of Experimental Terraforming Techniques
- Paper number
IAC-05-D4.1.06
- Author
Mr. Damian Rogers, Ryerson University, Canada
- Coauthor
Mr. Julio Aprea Perez, International Space University (ISU), The Netherlands
- Coauthor
Mr. Tobias Bittner, International Space University (ISU), Germany
- Year
2005
- Abstract
As a first paper to a two-part team project devoted to terraforming, this section, which included my personal contribution, was devoted to research on the feasibility of fundamental terraforming techniques for use on other celestial bodies. The focus here was on methods of terraforming bodies with different starting attributes and eventually achieving the desired end result of habitability by life - perhaps eventually human life. Main considerations were focused on ways in which to augment temperature, water levels, atmospheric composition, and atmospheric pressure. These four attributes are considered to be the main concerns when trying to define a habitable environment by our current understanding of life on Earth. It was found that a habitable environment would be one in which: (i) the yearly average global temperature of a planetary body should be between 0° and 30° C (with a maximum seasonal daily average of not less than -10° and not more than 40° C); (ii) available fresh water levels should be in the area of 10 L/person/day (including drinking, cooking, and cleansing estimates); (iii) a global average of 130 to 300 mbar of O2, 0.1 to 1 mbar of CO2, and enough N2 in order to act as a buffer for the atmosphere (though at least 10 mbar is needed); and (iv) an overall atmospheric pressure between 0.25 and 2.55 bar. When looking at these various needs for the existence of life, trends in terraforming techniques were found, which could solve several of these in parallel. It was found that importing volatile (NH3 or water) rich asteroids to a planet and impacting them could introduce N2 and NH3 into the atmosphere while at the same time act as a greenhouse gas to increase the global temperature and also provide a radiation shielding. This, in turn, can help to melt frozen stores of water ice, as is evident on some bodies, to provide the necessary fresh water supply. Another method, such as very large orbital mirrors, can help promote heating of the planetary surface and also contribute to melting frozen water ice or CO2 ice. Taking Mars as an example, calculations showed that a mirror of approximately 100 km radius would be needed to initiate a 5 K temperature increase for the poles. Therefore, it was seen that the most effective way of achieving all of the desired parameters would be to combine several methods to expedite the terraforming process. For instance, placing large orbital mirrors to heat a planet’s poles while at the same time importing large volatile rich asteroids would yield a much faster and more desirable result than either one of these methods could achieve alone. Therefore, in order to define a set path to follow in the way of terraforming a planet, these and other precursor activities must first be considered. Also, to undertake such large endeavors will require an increase in research in the appropriate fields such that these technological achievements can be realized. Currently, on-going research is being conducted in order to accommodate the final part to this team project, in which a more detailed look at a specific aspect of terraforming will be presented.
- Abstract document
- Manuscript document
IAC-05-D4.1.06.pdf (🔒 authorized access only).
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