Mars sample return

The U.S. Department of Energy and the National Aeronautics and Space Administration have both adopted this approach. For example, at the NASA Jet Propulsion Laboratory, the Dialogue process will be used in developing a Mars sample-return mission, which is scheduled for 2012. 

Mattingly, R., Matousek, S., Jordan, E Continuing evolution of Mars sample return. In 2004 IEEE Aerospace Conference Proceedings. 2004. 

MEPAG (2008) Science priorities for Mars sample return. Astrobiology, 8(3), 489-535. 

The instrument MIMOS II will be part of the upcoming ESA-NASA space missions ExoMars in 2018, and the Russian Space Agency sample return mission Phobos Grunt scheduled for launch in 2011 to visit the Mars moon Phobos. 

It is obvious from these experiments that the absorption spectrum of the Martian red surface can be simulated reasonably well by a non-unique variety of Fe rich phases or their mixtures as can the weak magnetism, so that a positive identification will probably only be possible, following further in situ analyses and/or sample return and analysis in the lab.Two Mars Exploration Rovers (MERs) are due to arrive at Mars in 2004 and will attempt to analyze rocks and soils on the surface using several small spectrometers, including PanCAM (an extended visible region spectrometer), MiniTES (a thermal emission spectrometer), APXS (alpha proton X-ray spectrometer measuring the major elements), Mossbauer (run at current local temperature), as well as a 5-level magnet array similar to that on-board the Pathfinder Lander. 

Different evolutionary histories of other terrestrial planets have influenced the relative concentrations of the transition elements compared to their cosmic abundances, as suggested by geochemical data for surface rocks on the Moon, Mars and Venus (Appendix 1). Chemical analyses of lunar samples returned from the Apollo and Luna missions show that minerals and glasses occurring on the Moon contain high concentrations of Fe and Ti existing as oxidation states Fe(II), Ti(III) and Ti(IV). Some lunar minerals, notably olivine and opaque oxides, also contain significant amounts of Cr(H), Cr(III) and Mn(H). The lack of an atmosphere on the Moon simplifies interpretation of remote-sensed reflectance spectra of its surface. 

Fuel generation from CO2 on Ft nanoparticle catalysts may be used to produce fuels electrochemically in Mars missions, from ambient CO2 and water, both present in the atmosphere and soils on Mars [112]. Such fuels made onsite would enable Earth-return propellants and life-support consumables [157,158]. Sridhar and co-workers [158] proposed a new architecture for an in situ propellant production plant, which utilises solid oxide electrolysis to accomplish the combined electrolysis of water and carbon dioxide. This system produces methane by means of a Sabatier reactor and oxygen via electrolysis in the optimal oxidiser-to-fuel mixture ratio. It also has the capability to produce additional oxygen for life support needs. Results demonstrate that combined electrolysis enables a competitive system for in situ resource utilisation, and is easy to be scaled for sample return from Mars and for possible human missions to the planet [158]. 

A collision with a Mars-sized object may have resulted in the formation of the Earth s moon. Our moon is by no means the largest satellite in the solar system, but it is unusual in that it and the moon of Pluto are the largest moons relative the mass of the planets they orbit. Geochemical studies of returned lunar samples have shown that close similarities exist between the bulk composition of the moon and the Earth s mantle. In particular, the abimdances of sidero-... 

The experiments were intended to clarify the question as to whether transmission of spores from Mars to Earth could be feasible. To do this, a Mars meteorite was simulated, i.e., the spores were mixed with powdered rock and the mixture pressed together to give a small cube about 1 cm3 in size. The spore concentration was about the same as in normal soil on Earth. The samples were in orbit for around 2 weeks, and their survival ability was determined on their return to Earth, compared with the corresponding samples which had been left on Earth (control experiment). 

Figure 1. Track of USNS Hayes leaving Mar del Plata, Argentina on February 1, (Julian Day 32) and returning February 19,1981. Circled numbers refer to oceanographic stations numbers along cruise track designate aerosol samples collected underway.

To date, there exists very little quantitative information concerning oxygen isotope compositions in major solar system reservoirs that is obtained by remote (spectroscopic) observation or spacecraft measurements. A measurement of water ice from comet P/Halley, made by the Giotto mission, yields = 12 75 %o (Balsiger et al. 1995 Eberhardt et al. 1995) but no measurement of is available. Precise data are obtained for the Moon, of course, from returned Apollo samples, and the oxygen isotope composition of Mars and the largest asteroid, Vesta, may be inferred from laboratory... 

Abstract NASA has used aerogel in several space exploration missions over the last two decades. Aerogel has been used as a hypervelocity particle capture medium (Stardust) and as thermal insulation for the Mars Pathfinder, Mars Exploration Rovers, and Mars Science Lander. Future applications of aerogel are also discussed and include the proposed use of aerogel as a sample collection medium to return upper atmosphere particles from Mars to earth and as thermal insulation in thermal-to-electric generators for future space missions and terrestrial waste-heat recovery technology. 

Since the amount of dust suspended in the Martian atmosphere varies a great deal by season, by altitude, and by latitude, the SCIM Mission would be planned so that it would arrive during the period of greatest atmospheric dust content and at the best altitude and latitude for maximum dust collection. The presence of a significant dust storm on Mars cannot be accurately predicted however, a dust storm would only increase the atmospheric dust content and thus the amount of sample collected and returned. 

Leshin L A, Clark B C, Forney L, Jones S M, Jurewicz A J G, Greeley R, McSween H Y, Richardson M, Sharp T, Thiemens M, Wadhwa M, Wiens R C, Yen A, Zolensky M (2003) Scienti-fic benefit of a Mars dust sample capture and Earth return with SCIM Lunar Planetary Sci. Conf.,XXXIV, Lunar Plane-tary Institute, Houston, TX Abstract 1288... 

---