The surface of Venus as revealed by Soviet Venera 9 and 10

Florensky, C. P.; Ronca, L. B.; Basilevsky, A. T.; Burba, G. A.; Николаева, О. В.; Pronin, A. A.; Trakhtman, A. M.; Volkov, V. P.; Zazetsky, V. V.

doi:10.1130/0016-7606(1977)88<1537:tsovar>2.0.co;2

Cited by 92 publications

(39 citation statements)

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“…The units identified on Beta are defined on the basis of their radar characteristics; the use of surface landers equipped with gamma-ray spectrometers and optical imaging systems provide ground truth of geochemistry, to determine rock types, and surface characteristics to assess the primary source of radar backscatter for these units. Within the portion of the equatorial region imaged by Arecibo are two Venera landers that provided both panoramic imaging and geochemical analysis of the Venus surface (Florensky et al, 1977). The northernmost lander, Venera 9 is located to the west of Devana Chasma (31.7" N, 298.8", with an uncertainty of approximately ?l" in both latitude and longitude) within an area mapped as a linear deformation zone on the eastern flank of Beta (Figure 6a).…”

Section: Frommentioning

confidence: 92%

“…The northernmost lander, Venera 9 is located to the west of Devana Chasma (31.7" N, 298.8", with an uncertainty of approximately ?l" in both latitude and longitude) within an area mapped as a linear deformation zone on the eastern flank of Beta (Figure 6a). The panoramic image of the surface indicates the presence of a large abundance of blocks and cobbles with sizes ranging from less than the resolution limit of the imaging system to up to 70 cm, with no apparent bedrock exposure (Figure 6b) (Florensky et al, 1977;Garvin et al, 1984). Although there is a relatively large uncertainty on the location of the lander, it is possible on the basis of its correspondence to units mapped from radar images to suggest a geologic setting to account for the observed surface features.…”

Section: Frommentioning

confidence: 99%

“…regional radar imaging, and the location of the lander on a slope (Florensky et al, 1977) we interpreted the large number of blocks and boulders at the Venera 9 site to be associated with deformation in the lineament belt forming talus deposits. Geochemical analysis of rocks by Venera 9 show them to have potassium, thorium, and uranium concentrations that are similar to terrestrial basalts with tholeiitic compositions (Florensky et al, 1977), suggesting that this may be a region of deformed volcanic plains.…”

Section: Frommentioning

confidence: 99%

“…Geochemical analysis of rocks by Venera 9 show them to have potassium, thorium, and uranium concentrations that are similar to terrestrial basalts with tholeiitic compositions (Florensky et al, 1977), suggesting that this may be a region of deformed volcanic plains. Located approximately 1700 km to the south of Venera 9 is the Venera 10 lander (16.0" N, 291.0", with an uncertainty of approximately * 1" in both latitude and longitude).…”

Section: Frommentioning

confidence: 99%

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Geology and tectonics of Beta Regio, Guinevere Planitia, Sedna Planitia, and Western Eistla Regio, Venus: Results from Arecibo image data

et al. 1991

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Section: Frommentioning

confidence: 92%

Section: Frommentioning

confidence: 99%

Section: Frommentioning

confidence: 99%

Section: Frommentioning

confidence: 99%

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Geology and tectonics of Beta Regio, Guinevere Planitia, Sedna Planitia, and Western Eistla Regio, Venus: Results from Arecibo image data

et al. 1991

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“…Surface erosion exists without doubt on Venus but its rate seems to be rather very low comparable with that on the lunar surface in the post-mare time than with the terrestrial or even martian rates. Existence of erosion on the surface of Venus has been proved through the analysis of TV panoramas sent to Earth by Venera landers (Florensky et al, 1977;Basilevsky et al, 1985). The observations have shown the presence of rock outcrops and loose soil with a trend for soil to occupy lows in the local topography at Venera 10, 13, and 14 sites as well as a rock-fragmented talus on the steep slopes of the Venera 9 site.…”

Section: Plate Tectonicsmentioning

confidence: 96%

Heat loss and tectonic style of Venus

et al. 1992

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The tectonic style of a terrestrial planet depends strongly on the mechanisms of heat release from the mantle through the lithosphere to the surface. Three types of lithospheric heat transfer have been proposed. (1) Lithospheric conduction, (2) (hot spot) volcanism, (3) plate recycling (mainly at spreading plate margins). In the case of the Earth the total heat flow is determined by plate recycling 65%) heat conduction through the lithosphere 20%, decay of radioactive elements in the crust 15%) hot spot volcanism ~1%. Scaling the mean surface heat flow density of the Earth to venusian conditions leads to 66mWlm'. In the case of Venus plate tectonics play only a minor role. Thus, two processes remain for heat release: (hot spot) volcanism and conduction. The term "hot spot" is written in brackets because volcanism on Venus occurs globally, not necessarily associated with hot spots.The volcanic lava production has been estimated from Venera 15/16 scenes. Arecibo and Magellan images revealed that the surface character south of 30" N is very similar to the area covered by Venera. The main results of the estimation are: (i) The maximum thickness of the plain lavas is 3 km. (ii) With plain lava thicknesses larger than 200 m the lava production from central volcanoes is negligible. (iii) Two age models have been used for the mean age of the area obseved: At, = lo9 a, At, = 400 x lo6 a. At, leads to the maximum lava production rate of 3 km3/a compared to 20 to 25 km3/a of the Earth; this gives a maximum contribution of 0.75 mW/m' to the heat flow density of Venus, i.e. about 1%. This implies that either heat conduction is the only dominating process for heat release or there is a hidden reservoir of the "missing basalt" somewhere or there is another unknown tectonic process. Assuming pure conduction and correcting the surface heat flow density for radioactive elements in the crust leads to a thickness of the thermal lithosphere of 45 km. A reservoir for the "missing basalt" could be basaltic underplating to a depth of 100 km. This gives a contribution of about 20 mW/m' with the age model At2 to the heat flow density from first order calculations.While the tectonic style of the Earth can be described to be linear formed at the plate margins, the surface of Venus is characterized by global spotty volcanism. The surface is more dominated by volcanic landforms than in the case of the Earth despite the relatively low lava production rate with a maximum of 3 km3/a. As plate tectonics is a minor process on Venus, conduction through a rather thin lithosphere should play an important role for heat release.

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Venus Missions

Moroz

Bazilevsky

2003

Encyclopedia of Space Science and Technology

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Launches of Soviet spacecraft to Venus were started in 1961. A full list of them is presented. The first success in space studies of Venus was achieved by the Soviets in 1967. Venera 4 reached the planet and fulfilled its mission. It was separated from the bus and entered the atmosphere, slowing as it descended. The parachute opened, and measurements of the atmospheric properties were taken down to an altitude 25 km above the surface. The probe was destroyed there due to high density and/or high temperature. Venera 4 was the first successful planetary atmospheric probe. The U.S. flyby probe, Mariner 5, arrived at Venus 1 day after Venera 4 and conducted some remote studies of the atmosphere. Then for about 10 years, NASA did nothing to explore Venus besides the Mariner 10 flyby on its way to Mercury. In contrast, the Soviet Union at that time was sending missions to Venus regularly, in the beginning using each astronomical window (about a 1.5‐year gap) and later each second window (about 3 years). This article briefly outlines the Soviet scientific output. Results of the studies include the atmosphere and its interaction with the solar wind and details on the surface of Venus. A lot of valuable information about Venus was obtained by the Soviet (and also U.S.) missions to this planet. Most of the data (although still not all) has been carefully analyzed. A set of new goals and new possibilities was identified by this activity. Possibly it is time now for a return to the exploration of Venus on a new level.

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The surface of Venus as revealed by Soviet Venera 9 and 10

Cited by 92 publications

References 6 publications

Geology and tectonics of Beta Regio, Guinevere Planitia, Sedna Planitia, and Western Eistla Regio, Venus: Results from Arecibo image data

Geology and tectonics of Beta Regio, Guinevere Planitia, Sedna Planitia, and Western Eistla Regio, Venus: Results from Arecibo image data

Heat loss and tectonic style of Venus

Venus Missions

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