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V * 495-69 1 b * ..-+* NASA TECHNICAL MEMORANDUM NASA TM 88495 ai! GEOLOGICAL-MORPHOLOGICAL DESCRIPTION OF THE LAKSHMI PLANUM (PHOTOMAP OF THE VENUSIAN SURFACE SHEET 8-4) A. A. Pronin et al. Translation of ttGeologo-morfologicheskoye opisaniye plato lakshmi (fotokarta poverkhnosti venery, list B-4)," IN: Astronomicheskiy vestnik, Vol. 20, No. 2, 1986, "Nauka" Press, MOSCOW, pp. 83-98 (UDC 523.42). DESCRIPTION(hASA-TM-8849 OF5) THE GEGLCGIC LAKSHflI AL-MCEL EIAhiUI! HOLOGICAL (FHO!IO?lBP N87-15926 I CE THE VENUSIAN SUBFACE SEEE'I E-4) (National Aeronautics and SFace Adaiaistration) 22 p Uncla E CSCL 03B G3/91 40324 NATIONAL AERONAUTICS AND SPACE ADMINISTRATION WASHINGTON, D.C. 20546 JANUARY, 1987 . STANDARD TITLE PAGE 1. Report No. 2. Govommont Accerrion No. 3. Rocipiont'r Catalog No. -NASA TM-88495 4. Titlo ond Subtitlo 5. Roport Dot. GEOLOGICAL-MORPHOLOGICAL DESCRIPTION OF THE January 1987 LAKSHMI PLANUM (PHOTOMAP OF THE VENUSIAN 6. Porforming Orgonixation Cod. SURFACE SHEET B-4) 7. Authodr) 8. Porforming Organixotion Report No. A. A. Pronin et al. 10. Work Unit No. 11. Contract or Grant No. 9. Performing Orgonixation Nom. ond Addroaa NASW-4006 The Corporate Word 13. Typo of Roport ond Poriod Covorod 1102 Arrott Building Pittsburgh, PA 15222 Translation 2. Sponroring Agoncy Nome and Addrors National Aeronautics .and Space Administration 14. Sponroring Agoncy Cod. Washington , D. C. 20546 5. Supplomontory Notes Translation of "Geologo-morfologicheskoye opisaniye plato lakshmi (fotokarta poverkhnosti vener'y, List B-4)", IN: Astronomicheskiy vestnik, Vol. 20, No. 2, 1986, "Nauka" Press, MOSCOW, pp. 83-98 (UDC 523.42) 16. Abatroct The morphological description of Lakshmi Planum and its surroundings is qiven: they are parts of a single striirture- It is su33cst& that the mechanism of plume ascent from Planetary interiors and its horizontal spreading is responsible far the structure formation. Folding and/or imbricating are the result of the process. Thus the Lakshmi structure can be considered a local center of radial spreading. The structure dimensions suggest that asthenospheric currents have been involved in its formation. ,Y in.-.. 17. Key Words (Selcctod by Author(s)) 18. Distribution Stotommt Unlimited .. 19. Security Ciaasif. (of thia roport) 20. Socurity Claarif. (of this pogo) 21. NO. of PO~OS 22. Prico Unclassified Unclassified 22 2 NASA-HQ GEOLOGICAL-MORPHOLOGICAL DESCRIPTION OF THE LAKSHMI PLANUM (PHOTOMAP OF THE VENUSIAN SURFACE SHEET 8-4)" A. A, Pronin et al. FOREWORD /83** One of the goals in radar mapping of Venus from the Venera- 15 and -16 unmanned interplanetary stations (AMS) is to create a series of photomaps and geological-morphological maps for the regions scanned. Maps of Venus' surface are created in separate sheets on map frames. Map sheet 8-4 covers the Lakshmi Planum in the center, framed by Venus' very large mountain structures -- the Akna and Freiya Montes to the northwest and north and the Maxwell Montes to the east. The southern framing of the planum is the Vesta Rupes. Corners of the map frame 8-4 have Venusian graphing coordinates: y1=80m, cp2=80, -60, y3=60, h,=?~oo, h 2- J3=300, cp4=60, h4=O0. When photomaps were created to overlap with related photomaps, their boundaries exceeded the limits of the area of the map frames established. PLOTTING PHOTOMAPS OF VENUS' SURFACE From November 1983 through July 1984, the Venera-15 carried out radar scanning of the northern regions of Venus' surface to about 30" latitude. Scanning and radio-profiling for height were done using a set of radar equipment including panoramic -/84 radar and a radar altimeter created in the Experimental Design Bureau of Moscow Power Engineering Institute. Signals reflected from the surface were processed, and individual radar panoramas * With this and the next article, the editors begin a series on creation of photomaps of the surface of Venus' northern hemisphere on the basis of materials from Venera-15 and -16. ** Numbers in the margin indicate pagination of the foreign text. 3 and profiles of surface heights were synthesized in the USSR Academy of Sciences Institute for Radio Engineering and Electronics (IRE). Radar panoramas were converted into cartographic projections and plan views of Venus' surface were created jointly by the IRE and the F. N. Krasovskiy Central Research Institute for Geodesy, Aerial Photography, and Cartography /l/. The M. V. Keldysh Institute of Applied Mathematic of the USSR Academy of Sciences precisely determined the station's movement and calculation elements of the orbit of photographic loops. Geological-morphological analysis was done in the USSR Academy of Sciences' V. I.Vernadskiy Institute of Geochemistry and Analytical Chemistry, as well as in the Academy's Geological Institute. Fig. 1. Breakdown of f8n O Venus' northern hemisphere into map f rames. When the 1:5,000,000-scale photomaps were created, the surface of Venus' northern hemisphere covered by radar scanning was arbitrarily divided into 27 map frames (fig. 1). Photomaps numbered from 8-2 to 6-27 were plotted in normal Lambert-Gauss conical projections in latitudes from 20 to 80'. To reduce distortion in the switch from a spherical surface to the map 4 plane for each 20-degree latitude belt, the values for the latitudes of two standard parallels on the cartographic projection were calculated. For the latitude belt from 60 to 80°, which includes photomap 8-4, values for the standard parallel latitudes are as follows: cp, =G3" 18'00,0", ~p2=7'i"30'00, I".) Entire photomaps are plotted on the basis of map frames by digital method using a computer and image output systems [l]. The digitizing cell on the photomaps corresponds to a locale of about 1 km. The position of relief cells on the photomaps is given in the Venusian graphic coordinate system recommended by the Working Group on Cartographic Coordinates and Elements of Planet and Satellite Rotation of the International Astronomical Union [4]. Readings of relief point heights are taken, as when cartographic projections are calculated, from the leveled spherical surface 605.1 km in radius used for Venus. MORPHOLOGICAL DESCRIPTION OF THE REGION Lakshmi Planum. For the most part, the Lakshmi Planum is, in plan view, an irregular hexagon with rounded corners and cross section of about 1,400 km, a trapezoidal projection to the north, and an extended projection to the east to the foothills of the Maxwell Montes (fig. 2). The planum's level surface is 4-4.5 km above the accepted leveled surface of Venus and is complicated by several small structures. These primarily include Colette in the center of the western half of the planum, which is extended along the meridian of an oval measuring about 130x80 km and about 2 km deep. Within up to 250 km of Colette there are narrow bands and scalloped areas of surfaces which appear bright to radar. These surfaces are oriented radially relative to the pater. On the whole, Collette, with a system of diverging flows, is a gigantic plate volcano about 600 km in cross section slightly extended at the meridian and occupying almost the entire western half of the Lakshmi planum (fig. 3). 5 /86 Fig. 2(a) There is another oval depression -- Sacajewea, measuring 200x120 km and about 1.5 km deep -- in the center of the western half of the plateau. It is oriented northeastward. The depression is less pronounced than Colette. Its presence is indicated not only by hypsometry, but also by two concentric light ovals and a horseshoe-shaped dark spot at its center. 6 t 1s TY -/87 Fig. 2(b) To the north of Sacajewea, a band of flat-topped uplands extends latitudinally across the entire eastern half of the plateau rising an average of 500 m above the floor of the plateau. The nature of the relationship of the plateau's plains material to that of the uplands along the irregular boundaries makes it possible to consider these uplands residual mountains. Their surface, marked by a diagonal grid of ridges and grooves apparently bears traces of earlier deformations which did not -/88 7 ORIGINAL PAN IS of wm Fig. 2. Photomap of Lakshmi Planum and surrounds. Contours indicate fragments shown in fig. 3-6; (a) diagram of planetographic names (b). Key: (1) Pomona Crown; (2) Dashkova; (3) Misne Canyon; (4) Worsar Scarp; (5) Viresacci Canyon; (6) Tessera Itzpapalotl'; (7) Freiya Montes; (8) Tessera Atropos; (9) Cotton; (10) Akna Montes; (11) Wanda Osipenko; (12) Rita; (13) Snow Maiden Plain; (14) Tessera Fortunae; (15) Semuna Ridge; (16) Cleopatra; (17) Maxwell Montes; (18) Otau Crown; (19) Ivka; (20) Zdravka; (21) Akhmatova; (22) Lakshmi Planum; (23) Magda; (24) Colette; (25) Zlata; (26) Sacajewea; (27) Rangrid Trenches; (28) Auski Ridge; (29) Siddons; (30) Lyudmila; (31) Tessera Clotho; (32) Berta; (33) Tamara; (34) Sigrid; (35) Danu Montes; (36) Vesta Rupes; (37) Tessera Moira. affect the younger plains deposits of the Lakshmi Planum. Mountains Framing the Lakshmi Planum. In the south, the main massif of the planum is framed by a belt about 100 krn wide (Danu Montes) consisting of linear ranges and valleys between 8 ORIGINAL PAM IS OF POOR QUALtl'V them, which are oriented almost everywhere along the edge of the planum. Individual ranges within the belt extend for tens of kilometers (to 100 km) in length and are 10-15 km wide. In relief, the 3-5-km-high Vesta Rupes, which is turned southward, corresponds to the belt of linear ridges so that the regional descent to the scarp rises in places above the planum's surface. The base of the scarp in places overlies the more southern area of unordered relief and conceals it (fig. 2). Fig. 3. Point where the Lakshmi Fig.
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