Mapping of Venus
This article may require cleanup to meet Wikipedia's quality standards. The specific problem is: Poor grammar and formatting inconsistent with the rest of Wikipedia. (January 2017) |
The mapping of Venus refers to the process and results of human description of the geological features of the planet Venus. It involves surface radar images of Venus, construction of geological maps, and the identification of stratigraphic units, volumes of rock with a similar age.
Satellite radar provides imagery of the surface morphology by using the physical properties of wave reflection. Long wavelength microwaves are used to penetrate the thick, cloudy atmosphere of Venus and reach to the surface. Different surface features reflect waves with different strengths of signal, producing images from which the maps are constructed.
After collection of the images of the Venusian surface, scientists started to map and identify different geologic materials and units according to distinctive surface features. Different groups of scientists analyzed different mapping areas, schemes and interpretation of features observed, to produce a classification of the units and comparison of their mapping.
Overview edit
Before the development of radar-based observation, the thick yellow Venusian atmosphere hid surface features.[1] In the 1920s, the first Venus ultraviolet project captured the thick atmosphere of Venus, but provided no information about the surface.
Venera program edit
From 1961 to 1984, the Soviet Union developed the Venera probes for surface mapping by radar. The Venera 4 (on October 18, 1967) was the first lander to make a soft landing on Venus (also the first for another planetary object). The probe operated for about 23 minutes before being destroyed by the Venusian atmosphere. The Venera series space probes returned radar images of the Venusian surfaces,[2] shown as below with the landing locations of the probes.
Magellan mission edit
The global surface of Venus was first mapped by the Magellan orbiter during 1990–1991 with 50 km spatial and 100 m vertical resolution. During three orbit regimes, the surface images were transmitted back to the Earth. These three orbiting motions of the spacecraft are called mapping cycle 1, 2 and 3.
During the mapping cycle 1 (left-looking) radar surface mapping on Venus (September 15, 1990 to May 15, 1991), around 70% of the Venusian surface was mapped by synthetic aperture radar. In cycle 2 (right-looking), 54.5% of the surface was mapped, mainly the south pole regions and gaps from cycle 1 during May 15, 1991 to January 14, 1992. Combining cycle 1 and 2 results in a total coverage of 96% of Venusian surface mapped. Cycle 3 (left looking) filled remaining gaps and collected stereo imagery of approximately 21.3% of the surface, increasing the total coverage to 98%.[3][4][5]
Proposed future InSAR mapping edit
The use of Interferometric synthetic aperture radar (InSAR) for mapping Venus has been proposed.[6]
Instead of surface mapping by SAR as done by previous missions, InSAR would measure the terrain motions during events such as earthquakes or tectonic movements. By performing the radar mapping at two separated times (before and after an event) over the same area, the terrain changes could be revealed.[6][7]
Mapping strategies edit
From the Magellan mission data, 3 types of images have been produced: (1) SAR images, (2) topographic images and (3) meter scale slope image.[7][8]
SAR imaging edit
SAR images provide the highest resolution data set. Microwave radiation is used to penetrate the thick atmosphere and map the surface of Venus.
The SAR images are black and white images, which show the surface features using the intensity of radar return (echo), either due to surface roughness or orientation.[7] For SAR imaging, spacecraft do not point directly downward (nadir) but slightly to the side—anywhere from about 10° to 45°. If the surface being mapped is smooth, the incident radar pulse will be reflected away from the spacecraft, resulting in a weak echo, which is represented by darker regions SAR images. On the other hand, if the surface is rougher, then more of the radar wave will be backscattered, and the intensity of echo will be stronger, which are represented by brighter areas in SAR images.
SAR images do not provide the color of surface, only the intensity of reflection of radar waves on the surface at a particular incidence angle. For example, when there is a light source shining on the blue cap on the left (left-looking), there will be shadows on the other side of the cap where light waves are blocked by the cap and no reflection occurs. If the looking direction is changed to the right, the shadowing (dark on SAR image) part will be at the opposite side.
The USGS Branch of Astrogeology[9] has produced full resolution radar maps (also known as FMAPs) of Venus from the SAR data collected from the mission, called the Magellan F-BIDRs (Full resolution Basic Image Data Records). The maps have a coverage of around 92% (combination of the 2 left-looking cycles).[3][10] The resolution is 75 m/pixel, which is the highest resolution Venusian map.
Topographic mapping edit
Topographic images were collected using radar altimetry. Compared to the SAR images, the topographic images have a significantly lower resolution of around 3–5 km/pixel. These images show lower elevations with darker pixels with higher elevations are shown with brighter pixels. Despite the low resolution, it is useful to study the regional feature of Venus, including initial evidence for the existence of rift zones.[7]
There are three types of topography on Venus
- Highlands with elevation greater than 3 km, cover about 10% of the surface
- Deposition plains with elevations around 0 to 2 km, cover more than 50% of the surface
- Lowlands (accumulation of eroded highlands) with negative elevation, cover the rest of the surface
The surface observation includes impact craters, volcanoes, and lava flow channels, which give clues to estimate the surface age, possible global resurfacing events, tectonic activities, internal structure and surface processes.
Unit classification and mapping schemes edit
Different missions have mapped different cartographic quadrangles of the surface of Venus. They applied different mapping schemes and came up with different classifications of Venusian units.
Here is a table comparing the different mapping scheme and unit identification by the Magellan science team (1994),[11] Vicki L. Hansen (2005)[12] and Mikhail A. Ivano and James W. Head (2011).[13] The possible matching of the above units are in accordance with their radar backscatter and surface features.
| Mapping Groups | Magellan Science Team (1994) | Mikhail A. Ivanov and James W. Head (2011) | Vicki L. Hansen (2005) |
|---|---|---|---|
| Mapping Scheme | Global-scale geologic mapping scheme (defined by difference in radar backscatter, surface texture and topographic) | Stratigraphic Classification Scheme (defined to global stratigraphy with a division of geologic time) | (defined by local formations and deformations, instead of global stratigraphic) |
| Unit Classification | Stratigraphic Units: | Stratigraphic Unit | |
| (Tessera is not in this classification) | 1. Tessera (t) | 1. Tessera terrain (Further classification into 7 types, according to the features in Hansen and Willis' paper in 1996[14]) | |
| 2. Mountain belts (mb) | |||
| 1. Lineated plains | 3. Densely lineated plains (pdl) | 2. Flow material from different origin locally | |
| 2. Reticulate plains | 4. Ridged plains (pr) | ||
| / | 5. Regional plains (rp, upper and lower units) | ||
| 3. Bright plains | / | ||
| 4. Dark plains | 6. Smooth plains (ps) | ||
| 5. Mottled plains | 7. Shield plains (psh) | ||
| 8. Shield clusters (sc) | |||
| 6. Digitate plains (lava flow fields) | 9. Lobate plains (pl) | ||
| Geomorphic units: | Structural features | ||
| 1. Complex ridged terrain (CRT or tesserae) | (Tesserae is a geological material instead of structural features) | ||
| 2. Ridged and fractured terrain | |||
| 3. Ridge belts (including mountain belts) | 1. Groove belt (gb) | 1. Secondary Structures | |
| 4. Fracture belts | |||
| / | 2. Rift zones (rz) | ||
| Deposits: - Associated with impact events | Impact Crater Forming Materials | ||
| 1. Crater material | 1. Crater materials (c) | 1. Crater material | |
| 2. Bright diffuse deposits | 2. Impact crater flow material (cf) | 2. Flooded crater material | |
| 3. Dark diffuse areas | |||
The details of the above mapping scheme and units will be discussed one by one below.
Geologic mapping scheme by the Magellan edit
The global-scale geologic mapping scheme by the Magellan science team was a very early mapping done by the Magellan mission (1990–1991). Instead of identifying different geological materials, it basically grouped the global surface units with different radar backscatter (white and dark in SAR images), topography and surface texture.
The mapped units and their characteristics are listed below.
Stratigraphic units edit
The stratigraphic units in this mapping scheme are classified as 6 types of plains:
| Stratigraphic units | |||
|---|---|---|---|
| Units | Radar backscatter | Surface features | Interpreted geological materials |
| Lineated plains | Moderate and homogeneous | Abundant fractures, forming grids or orthogonal patterns | / |
| Reticulate plains | Intermediate and homogeneous | Abundant and low sinuous ridges | / |
| Dark plains | Homogeneous, dark local areas | Smooth | Lava flow |
| Bright plains | Homogeneous, bright local areas | / | Lava flooding with extension and rifting |
| Mottled plains | Extensive areas with both bright and dark materials | Mottled textures with abundant small shields and despoites[clarification needed] | / |
| Digitate plains | Bright and dark deposites | In digitate patterns | Lava flow fields associated with coronae |
Geomorphic units edit
The units are defined by groups of structural features of commonly higher elevation area with ridges and deformations:
| Geomorphic units | ||||
|---|---|---|---|---|
| Units | Complex ridged terrain (CRT or tesserae) | Ridged and fractured terrain | Ridge belts | Fracture belts |
| Surface features | Ridges and fractures with deformations | Same as CRT, but with a single direction of deformations dominate | Linear, which parallel to the nearby ridges | Dense parallel linear fractures, mainly around equatorial and southern regions |
| Topography | Regional highland areas | Regional highland areas | Elevated ridges | / |
| Images | ||||
Deposits edit
The deposits are mainly the impact crater materials and its deposits:
| Deposits | |||
|---|---|---|---|
| Units | Radar backscatter | Surface features | Image |
| Crater material | Impact ejecta (bright) | / | |
| Bright diffuse deposits | Radar-bright materials | Forming "wispy patterns" | |
| Dark diffuse deposits | Radar-dark materials | Parabola in shape | |
Stratigraphic classification scheme edit
One way to do mapping on Venus and characterization on the geological units on Venus is by the stratigraphic classification scheme.[15] Mikhail A. Ivano and James W. Head (2011) mapped the area of geotraverses at 30°N[16] and 0°N. They traced and discussed the global spatial distribution of rock-stratigraphic units and structure, and suggested their time correlation and geological history.[13]
Stratigraphic units edit
This mapping scheme suggests that there are approximately 12 global stratigraphic units on Venus which are present on different quadrangles.[13] These stratigraphic units and landforms are listed below in terms of mechanism from the oldest to the youngest.
Tectonic units edit
Tectonic units are formations due to large-scale crustal processes. In this mapping scheme, these surface units are grouped into possible same set of geological materials, shown by similar surface features.
Tessera regions (t) edit
Tesserae are regions of heavily deformed terrain, mostly located on highland areas (greater than 2 km in elevation) on Venus. This tectonic feature -or uni— is thought to be the oldest material on Venusian surface with highest level of tectonic deformation.[17][18] It is of high topography and seen in white on the SAR images with high radar backscatter.[19] The materials composed tessa terrain, which was named as unit Tt in the mapping of V-17(Basilevsky, A. T.,1996).[20]
The intersecting of material and tectonic structures are the defined characteristic of tessera, but the sets are not always seen in the images.[13] Due to the heavy tectonic deformation, it contains both contractional features of ridges and extensional features of graben and fractures.[13]
The boundaries of tessera shows embayment by other materials of other units. By this cross-cutting relationship, it provides evidence of tessera being the oldest unit within the strata.[13]
Densely lineated plains edit
The densely lineated plains unit (pdl) is defined by the dense and parallel lineaments packed on the unit.[13] They make up a small area on Venus's global surface of around 7.2 x 108 km2.[13] The lineament is the pattern of deformation, which make it a typical structural–material unit.[13]
There is evidence showing the embayment of tessera by pdl's material in some tessera margins. Thus, it is possible that this unit is younger than the tessera unit.[13]
In SAR images, it also shows a high backscatter imagery, but lighter than that of tessera.
Ridged plains (pr) edit
The ridged plains unit are lava plains deformed by ridges. They have a smooth surface with relatively higher elevation than the surroundings.[13] The ridges are usually symmetrical in cross-section and collected into prominent belts.[21][22]
There is evidence in places showing that pr unit is embaying the t and pdl unit. Also, the deformation of pr took place after the formation of t and pdl units. Thus, pr unit is possibly younger than both unit t and pdl.[13] As most of the deformation features on pr is far away from that on t and pdl units, it is difficult to tell the age relationship of deformation directly.[23][24][25] However, there are some tessera-like deformations additional to the ridge belts, it suggests there are some possible overlapping of formation time in unit t and pr.[13]
In SAR images, pr units have noticeably higher radar backscatter than surrounding regional plains, but lower than tessera (t) and densely lineated plains (pdl) units. Ridges planes have older ages compared to surrounding regional plains (pr) due to the difference in radar albedo and embayment relationships suggested by McGill and Campbell (2006).[26]
The major occurrence of this unit is located among Vinmara, Atalanta, Ganiki, and Vellamo Planitiae, shich in a broad fan-shape,[27][28][29][30] and also appears between Ovda and Thetis Regiones and in the southern hemisphere within Lavinia Planitis.[31][32]
Some researchers mapped ridges of the pr unit as deformed structures instead of a unit.[33][34][35][36][37]
Mountain belts (mb) edit
The mountain belts unit is the only real mountain range on Venus in the area surrounding Lakshmi Planum, which covers only 1.3 x 106 km2 of the Venusian global surface,[27][38][39][40][41] while involves structural deformation of different materials in their formation.[13] There are in total four major mountain belts mapped on Venus, including the belts of Danu Montes, Akna Montes, Freyje Montes and Maxwell Montes (the highest mountain on Venus with elevation of around 12 km).[13]
When looking at the cross-cutting relationship, the inner ridges of the belts seems to be embayed by the material of regional plains (pr), which covered the plateau surface. There is later deformation in terms of tilting towards the belts and wrinkle ridges parallel to the belt. It suggested formation formed right before the deposition of regional plains and later deformation of the belts.[13]
Shield plains edit
The shield plains units (psh) refers to plains with volcanic edifices of shield-like features.[42][43][44] In most of the psh regions. the plains are concentrated and forms a group. It is the oldest unit in the strata showing no widespread deformation, in which only little tectonic deformation is observed, such as ridges and fractures.[13] Compared to the above units, this unit seems to cover a high proportion of the Venusian surface at around 79.3 x 106 km2. Although the distribution of psh is widely spread and homogeneous, there are also some regions with no psh units, including the Lakshmi Planum and some lowland of regional plains,[13] The shield plains are formed from shield domes over time and suggested that psh may be associated as volcanic plains with small sources of volcanic materials and mildly deformed by tectonics.[13]
There are embayment relationships, showing that this unit is younger than the above highly tectonized units (t and pdl) at a global scale. However, the absence of the unit in some regions makes this unit difficult to fit into the strata, especially between the highly tectonized units mentioned above, and regional plains which will be mentioned in the next section.[13]
In SAR images, the psh unit shows a higher radar backscatter compared to surrounding overlaying regional plains, still lower than units of t, pdl and pr.[13]
Regional plains (rp) edit
The regional plains unit (rp) is the most widespread unit on the Venusian surface of about 182.8 x 106 km2.[13] It is defined as smooth and homogeneous plains, which are deformed into networks of linear subparallel or intersecting ridges.[45] This unit is interpreted as having volcanic origin with deformation of wrinkle ridges superimposed. However, the source of volcanism is not obvious in the Magellan data.[13]
Regional plains are divided into abundant lower unit (rp1, Rusalka Formation) with smooth surface and relatively low radar backscatter and upper unit (rp2, Ituana Formation) with also smooth surface, but higher radar albedo. Wrinkle ridges heavily deform the lower unit while moderately deforming the upper unit. The lower unit is heavily tectonized and embayed by lava plains and flows. The younger upper unit is lacking in large heavily tectonized tessera regions.[13]
In SAR images, they show as an intermediate level of radar backscatter.
Shield clusters edit
The Shield clusters unit (sc) is similar to shield plains, but tectonically undeformed. Based on the analysis by Crumpler and Aubele (2000),[46] 10% of this unit shows evidence that it is younger than regional plains (rp).[47] Some of the small shield clusters are founded embaying the regional plains of both lower and upper layers, while in some regions, this unit is found on top of the rp unit and deformed together by wrinkled ridges.[13]
Smooth plains edit
The Smooth plains unit (ps) belongs to Gunda Formation, which is a smooth and featureless surface without tectonic marks. It only makes up about 10.3 x 106 km2 of Venusian surface. These plains are usually do not have impact craters, which is tectonic undeformed.[13] These plains are rarely with low domes. These suggested three type of setting for this unit:
(1) Many fields of smooth plains are near to the regions with young volcanism (such as Bell Regio) with the lobate plains (pl). However, the relationship of smooth and lobate plains is uncertain.
(2) Some of the unit is located as deposition around an impact crater, possibly associated with the impact events.[48][49]
(3) small ps units are inside the tessera regions (such as Ovda Regio), which may associate with a volcanic origin,
Due to the usual higher elevation of smooth plains, it is possible that the volcanic material of smooth plains is a younger unit.[13]
Lobate plains edit
The Lobate plains unit (pl) is a smooth surface crossed with some extension features associated with rift zones. These features make up to around 37.8 x 106 km2, which is significant. The origin of lobate plains is thought to be associated with large volcanoes, which sometimes appear with large dome-shaped rises.[13] One possible origin of this unit is from massive and multiple eruptions from large and localized volcanoes with little later extensional deformation.[13]
By cross-cutting relationships, the plains embay the wrinkle ridges containing regional plains, which suggested that lobate plains are younger.[13] However, as the lobate plains, smooth plains, shield cluster and rift zones are often seen as small fractures, it is difficult to tell their time relationship.
The SAR image shows uneven radar back-scatter flow-like pattern.
Structural Units edit
Structural units are formed due to deformation. The resultant properties depend on the stress applied to the formation and the stain of the rocks.
Tessera-forming structures (ridges and grooves) edit
Ridge structures are mainly discussed in the ridged plains (pr) part above.
Groove belts (gb) belong to the Agrona Formation, which refers to dense extensional structures. This unit appears to be sets of subparallel lineaments of fractures or grabens.[13] This deformation unit makes up to around 37.1 x 106 km2 of the Venusian surface. These fractures are the most obvious and are very abundant on the surface of Venus, and crosses different units on the surface. It appears to be a younger unit on the surface. However, some vast plains units are found embaying the grooves in some areas. It suggests the formation of gb unit before the formation of plains.[13]
The major difference between grooves unit and dense lineated plains are that the former is belt-like and the latter is patch-like.[13]
It is very important to map these fractures, as sometimes the rock unit may be too deformed and is not recognizable, which it can be mapped as "fractured plains materials" according to the guidelines of Wilhelms (1990).[50]
In SAR image, these fractures are of high radar albedo, as high as that of the tessera unit.[13]
Rift zones edit
The Rift zones unit (rz) belongs to the Devana Formation, which is also made up of dense extensional structures with defined numbers of fissures and troughs containing flat-floors.[13]
It is found that the rift zones are usually related to the lobate plains, which may indicate that the rifting is related to the young volcanism and also young volcanic plains formed.[13]
Impact Crater Forming Materials edit
Just like the impact craters on Earth and other terrestrial planetary bodies, impact craters on Venus include central peaks, rims, floors, walls, ejected deposits and outflows from the craters. There are two groups of materials, including undivided crater materials (c) and impact crater flow material (cf).[51]
The study of impact craters on Venus is important to discover its geological history. In testing the model of catastrophic and equilibrium Model (another hypothesis other than global stratigraphy[52]) on Venus, it is found that the older regional plains (rp) are embaying only around 3% of the impact craters and the younger lobate plains (pl) are embaying around 33% of the impact crater on Venus. It suggested that there are likely to have been at least two geological periods on Venus:
(1) Earlier global volcanic regime stage (Formation of older regional plains), when the high rate of volcanic activities overwrote the marks of impact cratering
(2) Later network-rifting and volcanic regime stage (Formation of younger lobate plains), when the intensity of volcanism is reduced and allowed more impact cratering to be left on the surface.
Thus, the studying of crater distribution and randomness may give clues for Venusian geological history.[53]
Global stratigraphy edit
Under the Global stratigraphic Classification Scheme, by correlating the units mentioned above (Mikhail A. Ivano and James W. Head, 2011),[13] the researchers suggested three phases of Venusian geological history:
(1) The earliest period, Fortunian Period, involved intensive formation of tessera (t) (building of thick crust at the same time).
(2) Then, it came to Guinevere Period, which firstly, there was formation of Atropos (dense lineated plains, pdl), Lavinia (Ridged plains, pr), Akna (Mountain belts, mb), and Agrona (groove belt, gb). Later, there was global emplacement of Accruva (shied plains, psh), Rusalka (lower regional plains, rp1), and Ituana (upper regional plains, rp2) Formations. There are events of wrinkle ridges formed around the global. Mostly of the surface of Venus was resurfaced in this period
(3) In the Altlian period, there are limited formations of smooth plains (ps), Gunda Formation, and shield clusters (sc), Boala Formation, possibly due to Atlian volcanism. There was significant reduction in the rate of volcanism and tectonism.[13] However, these proposed events, and formation of units are not yet fully explained by a complete Venus geological model, such as resurfacing of Venus or heat-pipe hypothesis.
The mapping scheme by Vicki L. Hansen (2005) edit
The mapping scheme applied by Vicki L. Hansen is mainly regional based, instead of using global stratigraphy as Mikhail A. Ivano and James W. Head did. This mapping scheme focuses on the regional origin of geological materials.[14]
Tectonic units edit
There are only two major units classified under this group. These two units are further classified below:[14]
Tessera Terrain edit
Tessera terrain is seen locally the oldest unit on Venus.
It can be further classified into eight groups according to the deformation features:[14]
- Fold Terrain
- "Lava Flow" Terrain
- S-C Terrain
- Extended Fold Terrain
- Folded Ribbon Terrain
- Basin-and-Dome Terrain
- “Star” Terrain
- Tessera Inliers
Some of the terrains have multiple deformations, but it is not essential for them to have complex deformation.[14]
Flow materials with different origins edit
The relatively low-lying plains are mapped as flows from different origins locally. These materials are thought to be thick young sediments deposited rapidly. In SAR images, the flows material can be radar-dark or bright.[14]
Structural features edit
Structural deformation is treated as a feature instead of a unit.[14]
There are some common features mapped, such as linear fractures, ridge and wrinkled ridge identified in many regions, and other local features only found in some regions, such as dome, belt fractures, ribbon, graben, etc.[14]
Impact crater-forming materials edit
The classification of impact crater-forming materials are (1) crater materials and (2) flooded crater materials,[12] which is similar to the stratigraphic classification scheme.
Differences between mapping schemes edit
Here are some differences on the terminology and classification of units:
(1) The term "complex ridged terrain (CRT or tesserae)"
(2) Treating tessera terrain as a global stratigraphic unit
(3) Terminology and classification of "plains"
The terminology of "complex ridged terrain (CRT or tesserae)" edit
Hansen (2005) suggested that the tessera terrain should not be named as "complex ridged terrain (CRT)". For the term "complex ridged terrain (CRT)" used by the Magellan science team (1994),[11] it carries confusions.[12] Ridges can be also understood as fold, which is a contractional feature. However, not all tessera deformation are due to contraction.
Treating tessera terrain as a global stratigraphic unit edit
For treating tessera terrain as the oldest global unit in the Stratigraphic Classification Scheme, it is questioned under Hansen (2005)'s mapping scheme.[12] Although it is commonly the oldest unit mapped in different Venusian areas, it may not be the case for everywhere. The assumption of all the tessera are formed at the same time and the oldest around the global are remained untested.
Terminology and classification of "plains" edit
There are a major difference in terminology between the Stratigraphic Classification Scheme and Hansen (2005)'s mapping scheme, which Hansen (2005) suggested that "fold material" should be used instead of "plains with different surface features". It can be explained by three reasons:[12]
- "Plains" is not used to describe geological material, but surface physical features.
- Also, according to fundamental geological mapping principles, secondary structure (such as lineated, ridged and wrinkled) should not be used to define geological units.
- There is no evidence that the Venusian plains are volcanic products resulted from extensive flood lava
Thus, in Hansen's mapping scheme (2005), plains are defined as flow from different local origins in regional mapping.
Quadrangles' mapping of Venusian geological units edit
The quadrangles mapping and classification of geological units by different groups of researchers are mainly based on regional units mapped locally. Different groups have their own grouping of units, which are not fully coherent with others work and the proposed global stratigraphy. Also, there are some regional features being classified regionally.
Cartography edit
The United States Geological Survey defines sixty-two cartographic quadrangles for the surface of Venus,[54] with V-1 as the north pole region and V-62 as the south pole region. Base on the FMAPs, different groups of Venus researchers are mapping different quadrangles for the surface of Venus, resulting in different type of units defined.
Here are some examples of quadrangle mapping and their ways of classifying and grouping observed geological units. Some of them are having a similar time sequence as the global stratigraphy mentioned above and will be highlighted below.
Examples of quadrangle mapping unit classification edit
Here are the list of examples comparing the mapping schemes and units in quadrangles (regional mapping):
| Quadrangles | Mapping group & year of publication | Mapping scheme | Stratigraphic units identified | Structural units mapped | Other information |
|---|---|---|---|---|---|
| V-5 Barrymore Quadrangle Mapping[55] | Elizabeth Rosenberg and George E. McGill, 2001 | Similar to the global stratigraphic mapping scheme with the oldest tessera, followed by dense lineated materials, up to other younger plains materials. |
|
| / |
| V-13 Nemesis tesserae quadrangle mapping[51] | Mikhail A. Ivanov and James E. Head, 2005 | Global stratigraphy units classification |
| / | / |
| V-35 Ovda Regio quadrangle mapping[56] | Leslie F. Bleamaster, III, and Vicki L. Hansen, 2005 | Mapping by grouping local formations and deformations, instead of global stratigraphic |
| / |
|
| V-48 Artemis Chasma quadrangle mapping[57] | Roger A.Bannister and Vicki L.Hansen, 2010 | Mapping by grouping local formations and deformations, instead of global stratigraphic |
| / |
|
Examples of regional geological mapping edit
Here is an example of geological map in quadrangle V-20. The units are classified as (1) tessera material, (2) plains materials, (3) materials of coronae and (4) materials of domes and miscellaneous flows, with structures like ridges, wrinkle ridge and lineations.
| Ｇeological map of V-20 | Original SAR image of V-20 |
|---|---|
References edit
- ^ Ross, F. E. (1928). "Photographs of Venus". Astrophysical Journal. 68–92: 57
- ^ Goldstein, R. M.; Carpenter, R. L. (1963). "Rotation of Venus: Period Estimated from Radar Measurements". Science. 139 (3558): 910–911.
- ^ a b Howington-Kraus, E., Kirk, R. L., Galuszka, D., & Redding, B. (2006). USGS Magellan stereomapping of Venus. In European Planetary Science Congress 2006 (p. 490).
- ^ "Mission Information: MAGELLAN". NASA / Planetary Data System. 1994-10-12. Retrieved 2011-02-20.
- ^ Grayzeck, Ed (1997-01-08). "Magellan: Mission Plan". NASA / JPL. Retrieved 2011-02-27.
- ^ a b Meyer, Franz J., and David T. Sandwell. "SAR interferometry at Venus for topography and change detection." Planetary and Space Science 73.1 (2012): 130–144.
- ^ a b c d Kazuo, O. "Recent Trend and Advance of Synthetic Aperture Radar with Selected Topics: Remote Sensing." (2013): 716–807.
- ^ Graff, Jamie R. MAPPING AND ANALYSIS OF THE TECTONO-MAGMATIC FEATURES ALONG THE HECATE CHASMA RIFT SYSTEM, VENUS. Diss. Carleton University Ottawa, 2014.
- ^ Herrick, R. R., & Sharpton, V. L. (2000). Implications from stereo‐derived topography of Venusian impact craters. Journal of Geophysical Research: Planets, 105(E8), 20245–20262.
- ^ Howington-Kraus, E., et al. "USGS Magellan stereomapping of Venus." European Planetary Science Congress 2006. 2006.
- ^ a b Senske, D. A., Saunders, R. S., & Stofan, E. R. (1994, March). The global geology of Venus: Classification of landforms and geologic history. In Lunar and Planetary Science Conference (Vol. 25, p. 1245).
- ^ a b c d e Hansen, V. L. (2005). Venus's shield terrain. Geological Society of America Bulletin, 117(5–6), 808–822.
- ^ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac ad ae af ag ah ai aj ak al Ivanov, Mikhail A., and James W. Head. "Global geological map of Venus." Planetary and Space Science 59.13 (2011): 1559–1600.
- ^ a b c d e f g h Hansen, V. L., & Willis, J. A. (1996). Structural analysis of a sampling of tesserae: Implications for Venus geodynamics. Icarus, 123(2), 296–312.
- ^ Basilevsky, Alexander T., and James W. Head. "The geologic history of Venus: A stratigraphic view." Journal of Geophysical Research: Planets 103.E4 (1998): 8531–8544.
- ^ Ivanov, Mikhail A., and James W. Head. "Geology of Venus: Mapping of a global geotraverse at 30 N latitude." Journal of Geophysical Research: Planets 106.E8 (2001): 17515–17566.
- ^ Ivers, Carol; McGill, George. "Kinematics of a Tessera Block in the Vellamo Planitia Quadrangle". Lunar and Planetary Science. 29
- ^ Hansen, Vicki; Willis, James (1998). "Ribbon Terrain Formation, Southwestern Fortuna Tessera, Venus: Implications for Lithosphere Evolution". Icarus. 132 (2): 321–343.
- ^ Bindschadler, Duane; Head, James (1991). "Tessera Terrain, Venus: Characterization and Models for Origin and Evolution". Journal of Geophysical Research. 96 (B4): 5889–5907.
- ^ Basilevsky, A. T. "Geologic mapping of V17 Beta Regio quadrangle: Preliminary results." Lunar and Planetary Science Conference. Vol. 27. 1996.
- ^ Frank, S.L., Head, J.W., 1990. Ridge belts on Venus: morphology and origin. Earth Moon Planets 50/51, 421–470
- ^ Kryuchkov, V.P., 1992. Ridge belts on plains. In: Barsukov, V.L., Basilevsky, A.T., Volkov, V.P., Zharkov, V.N. (Eds.), Venus Geology, Geochemistry, and Geophysics (Research Results from the USSR). University Arizona Press, Tucson, London, pp. 96–112
- ^ Gilmore, M.S., Head, J.W., 2000. Sequential deformation of plains at the margins of Alpha Regio, Venus: implications for tessera formation. Meteoritics Planet. Sci. 35, 667–687.
- ^ Ivanov, M.A., Head, J.W., 2001b. Geology of Venus: mapping of a global geotraverse at 30N latitude. J. Geophys. Res. 106, 17515–17566.
- ^ Basilevsky, A.T., 2008. Geologic map of the Beta Regio quadrangle (V-17), Venus. U.S. Geological Survey Sci. Inv. Map 3023
- ^ McGill, G.E., Campbell, B.A., 2006. Radar properties as clues to relative ages of ridge belts and plains on Venus. J. Geophys. Res. 111, E12006. doi:10.1029/ 2006JE002705.
- ^ a b Barsukov, V.L., Basilevsky, A.T., Burba, G.A., et al. (24 others), 1986. The geology and geomorphology of the Venus surface as revealed by the radar images obtained by Venera 15 and 16. J. Geophys. Res. 91, D399–D411.
- ^ Frank, S.L., Head, J.W., 1990. Ridge belts on Venus: morphology and origin. Earth Moon Planets 50/51, 421–470.
- ^ Kryuchkov, V.P., 1990. Ridge belts: are they compressional or extensional structures? Earth Moon Planets 50/51, 471–491.
- ^ Kryuchkov, V.P., 1992. Ridge belts on plains. In: Barsukov, V.L., Basilevsky, A.T., Volkov, V.P., Zharkov, V.N. (Eds.), Venus Geology, Geochemistry, and Geophysics (Research Results from the USSR). University Arizona Press, Tucson, London, pp. 96–112.
- ^ Squyres, S.W., Jankowski, D.G., Simons, M., Solomon, S.C., Hager, B.H., McGill, G.E., 1992. Plains tectonism on Venus: the deformation belts of Lavinia Planitia. J. Geophys. Res. 97, 13579–13599
- ^ Ivanov, M.A., Head, J.W., 2001a. Geologic map of the Lavinia Planitia Quadrangle (V-55), Venus. U.S. Geological Survey Sci. Inv. Map I-2684.
- ^ Johnson, J.R., Komatsu, G., Baker, V.R., 1999. Geologic map of the Barrymore Quadrangle (V-59), Venus. U.S. Geological Survey Sci. Inv. Map I-2610
- ^ Campbell, B.A., Campbell, P.G., 2002. Geologic map of the Bell Regio Quadrangle (V-9), Venus. U.S. Geological Survey Sci. Inv. Map I-2743.
- ^ Hansen, V.L., DeShon, H.R., 2002. Geologic map of the Diana Chasma Quadrangle (V-37), Venus. U.S. Geological Survey Sci. Inv. Map I-2752
- ^ McGill, G.E., 2004. Geologic map of the Bereghinya Planitia Quadrangle (V-8), Venus. U.S. Geological Survey Sci. Inv. Map I-2794.
- ^ Campbell, B.A., Clark, D.A., 2006. Geologic map of the Mead Quadrangle (V-21), Venus. U.S. Geological Survey Sci. Inv. Map 2897.
- ^ Pettengill, G.H., Eliason, E., Ford, P.G., Loriot, G.B., Masursky, H., McGill, G.E., 1980. Pioneer Venus radar results: altimetry and surface properties. J. Geophys. Res. 85, 8261–8270
- ^ Masursky, H., Eliason, E., Ford, P.G., McGill, G.E., Pettengill, G.H., Schaber, G.G., Schubert, G., 1980. Pioneer-Venus radar results: geology from the images and altimetry. J. Geophys. Res. 85, 8232–8260.
- ^ Head, J.W., 1990. Formation of mountain belts on Venus: evidence for large-scale convergence, underthrusting, and crustal imbrication in Freya Montes, Ishtar Terra. Geology 18, 99–102.
- ^ Pronin, A.A., 1992. The Lakshmi phenomenon. In: Barsukov, V.L., Basilevsky, A.T., Volkov, V.P., Zharkov, V.N. (Eds.), Venus Geology, Geochemistry, and Geophysics (Research Results from the USSR). University Arizona Press, Tucson, London, pp. 68–81.
- ^ Aubele, J.C., Slyuta, E.N., 1990. Small domes on Venus: characteristics and origin. Earth Moon Planets 50/51, 493–532.
- ^ Head, J.W., Crumpler, L.S., Aubele, J.C., Guest, J.E., Saunders, R.S., 1992. Venus volcanism: classification of volcanic features and structures, associations, and global distribution from Magellan data. J. Geophys. Res. 97, 13153–13197.
- ^ Guest, J.E., Bulmer, M.H., Aubele, J., Beratan, K., Greeley, R., Head, J.W., Michaels, G., Weitz, C., Wiles, C., 1992. Small volcanic edifices and volcanism in the plains of Venus. J. Geophys. Res. 97, 15949–15966.
- ^ Bilotti, F., Suppe, J., 1999. The global distribution of wrinkle ridges on Venus. Icarus 139, 137–157
- ^ Crumpler, L.S., Aubele, J., 2000. Volcanismon Venus. In: Sigurdson, H., Houghton, B., Rymer, H., Stix, J., McNutt, S. (Eds.), Encyclopedia of Volcanoes. Academic Press, San Diego, San Francisco, New York, Boston, London, Sydney, Toronto, pp. 727–770
- ^ Ivanov, M.A., Head, J.W., 2004b. Stratigraphy of small shield volcanoes on Venus: criteria for determining stratigraphic relationships and assessment of relative age and temporal abundance. J. Geophys. Res. 109, NE10001. doi:10.1029/ 2004JE002252
- ^ Campbell, D.B., Stacy, N.J.S., Newman, W.I., Arvidson, R.E., Jones, E.M., Musser, G.S., Roper, A.Y., Schaller, C., 1992. Magellan observations of extended impact crater related features on the surface of Venus. J. Geophys. Res. 97, 16249–16278
- ^ Izenberg, N.R., Arvidson, R.E., Phillips, R.J., 1994. Impact crater degradation on Venusian plains. Geophys. Res. Lett. 21, 289–292.
- ^ Wilhelms, D.E., 1990. Geologic mapping. In: Greeley, R., Batson, R.M. (Eds.), Planetary Mapping. Cambridge University Press, pp. 208–260.
- ^ a b Ivanov, Mikhail A., and James W. Head. Geologic Map of the Nemesis Tesserae Quadrangle, V-13, Venus. US Department of the Interior, US Geological Survey, 2005.
- ^ Hansen, Vicki L. "Venus's shield terrain." Geological Society of America Bulletin 117.5–6 (2005): 808–822.
- ^ Ivanov, M. A., and J. W. Head. "Volcanically embayed craters on Venus: testing the catastrophic and equilibrium resurfacing models." Planetary and Space Science 106 (2015): 116–121.
- ^ Tanaka, Kenneth L., et al. The Venus geologic mappers' handbook. No. 93-516. US Geological Survey, 1993.
- ^ Rosenberg, Elizabeth, and George E. McGill. Geologic map of the Pandrosos Dorsa quadrangle (V-5), Venus. US Department of the Interior, US Geological Survey, 2001.
- ^ Geological Survey (US), Leslie F. Bleamaster, III, and Vicki L. Hansen. Geologic map of the Ovda Regio Quadrangle (V-35), Venus. US Department of the Interior, US Geological Survey, 2005.
- ^ Bannister, Roger A., and Vicki L. Hansen. Geologic map of the Artemis Chasma Quadrangle (V-48), Venus. US Department, of the Interior, US Geological Survey, 2010.