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General Disclaimer One Or More of the Following Statements May Affect General Disclaimer One or more of the Following Statements may affect this Document This document has been reproduced from the best copy furnished by the organizational source. It is being released in the interest of making available as much information as possible. This document may contain data, which exceeds the sheet parameters. It was furnished in this condition by the organizational source and is the best copy available. This document may contain tone-on-tone or color graphs, charts and/or pictures, which have been reproduced in black and white. This document is paginated as submitted by the original source. Portions of this document are not fully legible due to the historical nature of some of the material. However, it is the best reproduction available from the original submission. Produced by the NASA Center for Aerospace Information (CASI) Technical Report 1,'isitimg-Odduate Fellow at the Lunar and Planetary I stitute 6 June 1983 - 15 December 1983 MARTIAN IMPACT BASINS: MORPHOLOGY D T.FFERENCES AND TECTONIC PROVINCES. Marianne Stam*, Peter H. Schultz**, and George E. McGill* (*Dept. of Geology and Geography, Univ. of Massachisetts, Amherst, MA 01003; **Lunar and Planetary Institute, 3303 NASA Road 1, Houston, TX 77058) Detailed geomorphic and structural mapping of five martian basins and preliminary study of eleven other basins reveal four characteristic styles of modification that relate to the degree and age of past tectonic W activity. Within regions that exhibit no evidence for tectonic activity bo ("inactive"), the modification style can be used to distinguish areas (J,° dominated by different exogenic processes. 'This study provides a framework 1 [ for understanding these different styles of basin modificaticn (1). Basins in regions that have experienced extensive tectonic activity ("active") consist of two types that depend on whether the structures s present are due to extension or to compression. Al Qahira, Aram Chaos, rn Chryse, Ladon, and Mangala are in extensional crustal regimes; they are characterized by chaotic terrain, well developed runoff and outflow chan- aa craters rn nels, numerous floor-fractured (Table 1) and, with the exception 0 of Mangala. (which is largely obscured), ?ow ring-spacing values. These ,. a geomorphic characteristics vary somewhat among the five basins, perhaps Ln z ^ as a function of relative distance from Tharsis and Elysium. For example, H U Al Qahira is much closer to the older Elysium province than are Ladon 4 ;) R and Aram Chaos, and the latter two have be ter preserved floor-fractured z cratt-r-s, chaotic terrain, and outflow channels. From counts of craters N 75ki. in diameter, the chaotic terrain associated with Al Qahira is older than that associated with Ladon. These observations a e consistent with modification of the basins at different times; earlier for basins closer to the older center of tectonic activity, Elysium. As a group, these A ^^ Z z five basins appear to have suffered the most endogenic modification of q Z m an Y on M ^rs. This is inferred to be the result of their settingsg s within areas dominated by relatively recent extensional tectonics. tiu I Sirenum basin is located in an "active" crustal region with NW-SE 14 trending ridges believed due to compressional tectonics. Sire p um is w V degraded, with many heavily and lightly furrowed areas and furrowed ,-..1a IJ raters.c A large compressional ridge system collars the western portion -I ^ N o y 7 — of its innermost ring (2). Chaotic terrain and outflow and runoff channels are absent, and floor-fractured craters are rare, in contrast to the r- ^+ rejuvenated basins of the extensional regions near Tharsis and Elysium. i4 w ,^ South of Lyot and Deuteronilus A and B ("active/inactive"), found U c v on the martian crustal dichotomy boundary, are characterized by planated -+ or inverted topography, fretted terrain, and "fretted channels" (3). :14 _ e They appear to have undergone complete planation, or were filled completely ;a` '^ and later exhumed by mass wasting processes (1). Their complex history suggests extensive endogenic modification in thw-' past but relatively "inactive" conditions now. Presently, the morphologies of these basins are dominated by exogenic (periglacial?) processes. ­ Basins in "inactive" crustal regions are characterized by a mantled appearance or by heavily furrowed and channelled basic rims." (Table 1). Cassini and Cassini A are heavily mantled basins,N Wth rings expressed by furrowe-' scarps rather than massifs or knobs. Th g-;f^rt••owing is inferred R. to result from a mass-wasting process that "pasgiVe "" re}ji'venates the mantled rings (1). In other "inactive" crustal zones, basins are charac- terized by heavily furrowed and channelled rims, and 4-hIgh ring-spacing r averages. Examples include: Schiaparelli, Huygens, Overlapped by Newcomb Crater, Overlapped by Schiaparelli, and West of Le Verrier (Table 1). Unlike the Cassini basins, these structures are mostly modified by erosional processes. Fu:cowing and channelling preserve the identy of their ring s:arp forms while, at the same time, these processes are back- wasting the scarps. These basins are located in an "inactive" crustal r4,gion that is relatively old and is or was volatile rich. In conclusion, martian impact basins express at least four major styles of modification. These styles of rejuvenation and degradation are important indicators of: 1) the intensit: r and age of past tectonic activity, 2) whether the tectonic activity was extensile or compressive, and 3) the types of exogeni(. processes that dominate in different stable crustal regions on Mars. 1 +01 k 1 run llrrrxrn.w4 Cku (l.+nl I7rUrrr 16 l 11th.— I lm l • fr4rn •Rrry w CrnKr, KI ('r 111wryur.nrry Irnwq. CIV.uI 0avn Ilumrrr JO Im M • R^rynrinlr yu.,n, d TAarv. 14 fJw11m Ylury \ame. 1.\4uw 11m1 110•Im Rrry. InJr. ho.. ►rtnlrrr (lKrr Kraw^ -- _. — L (,Enna I*I N 2115 '17b 42 r 0 4 199 46fN 2910 (bola Km.^ - lram 17K.. 21 t .1 7 \ 450 4 1 NI 5370 9934 0.du. .+.. I. I. 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Ihrrl.p(N n. 1 \1 224 IM 11 2 209 0197 90W II.a.J1 '-1, 4...nn l r•Kr Iwn.waJ n. rrp fYN n. 1 1405 V, 5 S 4x0 1 V0 7016 7592 E Cwl.:dlr \nuryrrdl, L412 W.22 S 442 2 I VV 7M5 7411 Ikeda w rlunrrlld nm. - Mru r11r SrnKr lb M'. 17 5 4.10 1 0b) 0597 -- I#VKr.rnJlr A 42 M' 44 \ 2110 — --- - 4 194 0929 57114 M.rrtnd. plarr- W 1r.1.^n(41. 4.1nr I1r.Kr,wJ... 0' 110 w 425 % 201 in1 71.1 $711 krurd mnrn Inr e.r vvll. 1..+ 122 W 410 \ $70 0 154 %075 5100 'lJrOm.( .(- I rt". nar.n 1. k knwl S'0WU 461 Byrn l 19841 r U.lnrrr..Irrrrrlrrrd In•n Inn ..^► AR .w1rn Invn rnlrr 4AW1r. n V 119021 u fnVl 119191 ^11.n pnmaKr rylrl. 1hr hSax W Ow /nM 1.,,„ Rrry Junrrr .. Rr1a11.r narWl p.rl.w rr 4 my IN a V" barn Cahn PA. 1901 (1) Schultz, P.H., Schultz, R.A. and Rogers, J. (1982)_."Jour.• Geophys. Research, p. 9803-9820. (2) Chicarro, A.F. Schultz, P.H., and Masson, P. (1983) Lunar and Planetary Science XIV, p. 88-999 -_Lunar and Planetary Institute, Houston. (3) Sharp, R.P. and Malin, M.C. (1975) Geol. Soc. Amer. Bull., 86, p. 593-609. (4) Croft, S.K. (1979) UCLA Ph.D. Disser- tation. (5) Pike, R.J. (1981) Rpts. of Planetary Geology Program, NASA TM 84211, p. 123-125..
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