By National Research Council, Division on Earth and Life Studies, Board on Life Sciences, Division on Engineering and Physical Sciences, Space Studies Board, Committee on an Astrobiology Strategy for the Exploration of Mars
3 contemporary advancements have vastly elevated curiosity within the look for existence on Mars. the 1st is new information regarding the Martian surroundings together with proof of a watery earlier and the potential for atmospheric methane. the second one is the opportunity of microbial viability on Mars. ultimately, the imaginative and prescient for area Exploration initiative incorporated an specific directive to look for the proof of existence on Mars. those medical and political advancements led NASA to request the NRC's guidance in formulating an up to date built-in astrobiology process for Mars exploration. between different subject matters, this file offers a evaluation of present wisdom approximately attainable existence on Mars; an astrobiological evaluation of present Mars missions; a evaluate of Mars-mission planetary safeguard; and findings and suggestions. The file notes that the best bring up in realizing of Mars will come from the gathering and go back to Earth of a well-chosen suite of Martian floor fabrics.
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Extra resources for An Astrobiology Strategy for the Exploration of Mars
The concept of survival energy, that which is required for repair of macromolecules, maintenance of ion gradients, and so on,2 implies that life could survive, although not multiply, in a much wider range of environments than was formerly thought possible. The availability of nutrient elements may also impose limits to life. As mentioned in Chapter 1, it is reasonable to assume that martian life, if any, would be based on carbon (C), hydrogen (H), nitrogen (N), oxygen (O), phosphorus (P), and sulfur (S).
E. L. S. G. Strom, “Evidence for Ancient Continental Glaciation in the Martian Northern Plains,” Journal of Geophysical Research 100:5351-5368, 1995. 37. H. Y. 2006; and references therein. 38. H. , 2006. 39. H. Y. 2006; and references therein. 40. J. Bibring, Y. F. Mustard, F. Poulet, R. Arvidson, A. Gendrin, B. Gondet, N. Mangold, P. Pinet, F. Forget, and the OMEGA team M. Berthé, J. Bibring, A. Gendrin, C. Gomez, B. Gondet, D. Jouglet, F. Poulet, A. Soufflot, M. Vincendon, M. Combes, P. Drossart, T.
C, H, N, O, P, and S have all been detected on Mars. 3 The martian atmosphere contains only 160 microbars (mbar) of N2, and nitrates have not been detected in the soils. Much of the original nitrogen inventory could have been lost by impact erosion of the atmosphere during heavy bombardment, subsequent sputtering by the solar wind, or photochemical processes. Access to organic carbon is another potential problem. While CO2 is the dominant species in the atmosphere, reduced carbon compounds may be rare at the surface, despite continual delivery of organic compounds to the martian surface in meteorites and interplanetary dust particles.
An Astrobiology Strategy for the Exploration of Mars by National Research Council, Division on Earth and Life Studies, Board on Life Sciences, Division on Engineering and Physical Sciences, Space Studies Board, Committee on an Astrobiology Strategy for the Exploration of Mars