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Isotopic Composition of the Martian Atmosphere Author(S): Alfred O

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Isotopic Composition of the Martian Atmosphere Author(S): Alfred O Isotopic Composition of the Martian Atmosphere Author(s): Alfred O. Nier, Michael B. McElroy and Yuk Ling Yung Reviewed work(s): Source: Science, New Series, Vol. 194, No. 4260 (Oct. 1, 1976), pp. 68-70 Published by: American Association for the Advancement of Science Stable URL: http://www.jstor.org/stable/1742562 . Accessed: 18/01/2013 12:54 Your use of the JSTOR archive indicates your acceptance of the Terms & Conditions of Use, available at . http://www.jstor.org/page/info/about/policies/terms.jsp . JSTOR is a not-for-profit service that helps scholars, researchers, and students discover, use, and build upon a wide range of content in a trusted digital archive. We use information technology and tools to increase productivity and facilitate new forms of scholarship. For more information about JSTOR, please contact [email protected]. American Association for the Advancement of Science is collaborating with JSTOR to digitize, preserve and extend access to Science. http://www.jstor.org This content downloaded on Fri, 18 Jan 2013 12:54:12 PM All use subject to JSTOR Terms and Conditions in B2, being smaller than those in land at any other site could result in a prelanding observations. These results B3, were better covered by the bigger landing delay and significant additional will be reported on when completed. Ten- dunes apparent in the B2 pictures, and operational complexity. Acceptance of tatively, Viking 2 rests in a deflation that the smaller dunes in B3 might not this additional complexity was not justi- hollow. cover the ejecta from the larger craters fied, based on the B3 assessment cited H. MASURSKY there as well. Site B3 was favored by above. U.S. Geological Survey, still others independent of the dune argu- Subsequently, the B3 a and / ellipses Flagstaff, Arizona 86001 ment since it appeared to them that B3 (Fig. 8) were coalesced into one with pre- N. L. CRABILL was smoothed by uniform mantling. liminary coordinates of 48?N, 226?W. Fi- NASA Langley Research Center, In the B sites, where dunes and aeo- nal coordinates (47.89?N, 225.86?W) were Hampton, Virginia 23665 lian mantle were observed, an attempt selected on 30 August after review of the References and Notes was made to estimate thickness of cover rev 20 stereoscopic coverage. Detailed 1. H. Masurskyand N. L. Crabill,Science 193,809 based on dune spacing and dune slopes. mosaic of the landing site with the lander (1976). The minimum thickness was estimated dispersion ellipse is given in Fig. 10. 2. C. B. Farmer,personal communication. 3. G. Schaber,J. Boyce, A. Dial, M. Strobell,and as being adequate to cover small crater The crater Mie east of the landing G. Stewartprovided near-real-time crater count- ing and analysesfor these and many other loca- ejecta. Estimating impact crater ejecta point is covered with larger dunes and tions. block size at two crater diameters from deflation hollows (Fig. 11), and the polyg- 4. H. Kieffer,personal communication. 5. The Viking 2 site certificationeffort was a team the crater Mie (100 km in diameter) was onally fractured lava flows west of the effortas it was for the Viking1, except thatinfra- difficult. The estimated 10-m block size site (Fig. 12) are covered with a thin man- red observations rather than radar data were used in conjunctionwith imagesto evaluatethe was based on ejecta sizes measured in the tle of wind-blown material that partially sites. H. H. Kiefferand his associates reduced 7 site and fills the fractures. At the south end of the infraredthermal mapperdata and made them Surveyor landing Apollo 15, availablein near real time to help in site evalua- Apollo 16, and Apollo 17 high-resolution B3 region, a large channel (Fig. 13) dis- tion. C. B. Farmerand his teamsimilarly reduced The block de- sects and crosses the 600 the Mars atmosphericwater data very expedi- photographs. populations area, extending tiously. Hazard analyses were done by J. A. pend on the number of small craters be- km to the south toward the Elysium vol- Cutts, K. W. Farrell,L. Crumpler,T. Spudis, and E. Theilig. Geologicaland terrainanalyses low the resolution limit that may exca- canoes. Some of the large craters (Fig. 14) were performedby J. E. Guest, R. Greeley, vate blocks from below the wind-laid are extensively modified by wind erosion, G. Schaber, J. Boyce, J. A. Cutts, K. W. Farrell, M. H. Carr, and L. Soderblom. mantle and the number exposed by defla- possible water sapping, and dissection, so Imagedata processing proceeded through a com- tion. were deemed as that their blankets are etched out plicatedchain with the help of R. Johansen,M. Slopes acceptable ejecta Martin,and associates at the Mission and Test based on Earth analogs, except on the in negative relief. The area is thus partial- ImagingSystem Facility;G. Traverand associ- inner of craters. mantled aeolian material in the ates at the Mission and Test Photoprocessing margins ly by System; R. Ruiz and associates at the Image The infrared thermal mapper results north, where the landing site is located, ProcessingLaboratory; J. Hewittand associates at the JPL photo laboratory;and R. Tyner and for the B2 region indicated low thermal and stripped in the south. The crater W. Sowers (who madephotographic mosaics as inertia and large amounts of fines (4). No counts previously cited confirm this in- fast as these images were delivered). L. B. Garrett and others organized this image pro- data were available for the specific can- terpretation. cessing system; and D. Roos monitoredits day- didate The thermal inertia at B3 The conclusion of the search for the to-day implementation.Thanks are also due to ellipses. M. J. Alazard, D. L. Anderson,G. A. Briggs, was determined to be approximately sim- Viking 2 site was the selection of the B3 D. M. Davies, J. D. Goodlette,R. Hargraves,S. L. Hess, L. Kingsland,T. Z. Martin, W. H. ilar to that at the Viking 1 site; the re- site in Utopia Planitia. The landing was Michael, H. J. Moore, II, E. C. Morris,T. A. quired noon coverage was not available successfully accomplished at 3:58:20 Mutch,F. T. Nicholson,W. J. O'Neil, T. Owen, F. D. Palluconi,J. D. Porter,R. J. Reichert,C. (4). p.m. P.D.T., earth received time, on 3 Sagan, R. W. Sjostrom, B. A. Smith, C. W. Observations showed more atmospher- September 1976. Snyder,G. A. Soffen,T. E. Thorpe,P. Toulmin III, E. D. Vogt, and the rest of the VikingFlight ic water at B2 than at B3 (2). There was a Studies are under way to compare the Team at Jet PropulsionLaboratory and the U.S. diurnal variation in water content actual conditions encountered at both GeologicalSurvey at Flagstaff.As before, J. S. greater Martin,Jr., A. T. Young,and B. G. Lee provided at B2 and it had an assumed 10? warmer the Viking 1 and Viking 2 landing sites a readyhand at the Vikingtiller. surface temperature, although no data with those expected on the basis of the 2 September1976 were available at the site. These factors were carefully weighed; and the B3 site was selected for the fol- lowing reasons. 1) Safety. It appears that B3 is ade- Isotopic Composition of the Martian Atmosphere quately mantled, muted, and filled. Site B2 may be as good, but the seeing due to Abstract. Results from the neutral mass spectrometer carried on the aeroshell of clouds and imaging quality diminishes Viking 1 show evidence for NO in the upper atmosphere of Mars and indicate that the confidence in the coverage. Site B3 ap- isotopic composition of carbon and oxygen is similar to that of Earth. Mars is en- pears more homogeneous throughout the riched in 15Nrelative to Earth by about 75 percent, a consequence of escape that area of the 99 percent ellipse. implies an initial abundance of nitrogen equivalent to a partial pressure of at least 2 2) Science. There is a small distinc- millibars. The initial abundance of oxygen present either as CO2 or H20 must be tion between the sites. The warmer tem- equivalent to an exchangeable atmospheric pressure of at least 2 bars in order to in- perature at B2 is in its favor. The water hibit escape-related enrichment of 18O. content difference was not deemed signif- icant. The most significant scientific dis- Viking 1, whichlanded on Mars on 20- the planet's surface (1). A preliminary ac- tinction had already been realized when July 1976, included as part of its scientif- count of the results has been published the northern latitude band was selected. ic payload a mass spectrometer designed (2). The martian atmosphere consists 3) Operations. Implementation is to measure properties of the neutral at- mainly of CO2, with traces of N2, Ar, O2, straightforward at B3. The additional mosphere between about 100 and 200 km CO, and 0. The relative abundances of data analysis and acquisition required to during the descent of the spacecraft to oxygen and carbon isotopes in the mar- 68 SCIENCE, VOL. 194 This content downloaded on Fri, 18 Jan 2013 12:54:12 PM All use subject to JSTOR Terms and Conditions 12cI80 Fig. 1. Mass spectrumshowing various mass peaks (amu)as spectra are scanned. Since time also increases to the right (5 seconds per scan), the spectrum includes a distortion due to the increase in 12c ambient pressure during the time of a spectral scan. Thus, for ex- ample, the 12-amupeak due to 12Cfrom CO2is 1.4 times higher,when referredto the 44-amupeak, than it would have been had the spec- trum been scanned at constant altitude.
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