Rheasilvia
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Southern hemisphere of Vesta, showing Rheasilvia crater
LocationAsteroid Vesta
Coordinates75°S 301°E / 75°S 301°E / -75; 301[1]
Diameter505 km (314 mi)
DimensionsOne of the tallest known mountains in the Solar System
Peak20–25 kilometres (12–16 mi; 66,000–82,000 ft)[2][3]
DiscovererHubble Space Telescope
EponymRhea Silvia, a mythological vestal virgin and mother of the founders of Rome, Romulus and Remus

Rheasilvia /ˌriːəˈsɪlviə/ is the most prominent surface feature on the asteroid Vesta and is thought to be an impact crater. It is 505 km (314 mi) in diameter, which is 90% the diameter of Vesta itself, and is 95% the mean diameter of Vesta, 529 km (329 mi). However, the mean is affected by the crater itself. It is 89% the mean equatorial diameter of 569 km (354 mi), making it one of the largest craters in the Solar System, and at 75°S latitude, covers most of the southern hemisphere. The peak in the center of the crater is 200 km (120 mi) in diameter, and rises 22.5 km (14.0 mi; 74,000 ft) from its base,[3][2] making it one of the tallest mountains known in the Solar System.

Discovery

Rheasilvia was discovered in Hubble Space Telescope images in 1997,[4] but was not named until the arrival of the Dawn spacecraft in 2011. It is named after Rhea Silvia, a mythological vestal virgin and mother of the founders of Rome, Romulus and Remus.[1]

Characteristics

The crater partially obscures an earlier crater, named Veneneia, that at 395 km (245 mi) is almost as large.[5]

Rheasilvia has an escarpment along part of its perimeter which rises 4–12 km (2.5–7.5 mi) above the surrounding terrain. The crater floor lies about 13 kilometres (8.1 mi) below the surrounding surface. This basin consists of undulating terrain and a central mound almost 200 km (120 mi) in diameter, which rises 20–25 km (12–16 mi; 66,000–82,000 ft) from its base,[3][2] one of the tallest known mountains in the Solar System, and possibly formed due to a planetary scale impact.[6]

Spectroscopic analyses of Hubble images have shown that this crater has penetrated deep through several distinct layers of the crust, and possibly into the mantle, as indicated by spectral signatures of olivine.[7]

Vesta has a series of troughs in an equatorial region concentric to Rheasilvia. These are thought to be large-scale fractures resulting from the impact. The largest is Divalia Fossa, approx. 22 km (14 mi) wide and 465 km (289 mi) long.

It is estimated that the impact responsible excavated about 1% of the volume of Vesta, and it is likely that the Vesta family and V-type asteroids are the products of this collision. If this is the case, then the fact that 10-km fragments have survived bombardment until the present indicates that the crater is at most about 1 billion years old.[8] It would also be the origin of the HED meteorites. Known V-type asteroids account for 6% of the ejected volume, with the rest of the fragments presumably either too small to observe, or removed from the asteroid belt by approaching the 3:1 Kirkwood gap, by the Yarkovsky effect, or (in the case of small fragments) by radiation pressure.

Gallery

Elevation map of Vesta's southern hemisphere. Higher elevations (red) are found on the crater rim (occluding Veneneia) and the central peak.
Outlines of Rheasilvia and Veneneia, the latter being partially obliterated by the former.
Hubble image of Vesta from May 2007. The flat spot at lower right is Rheasilvia seen in profile.
Computer-generated oblique view of Rheasilvia, with color-coded elevation in the lower version. A flyover video is available at the source.
Shaded-relief topographic map of Vesta's southern hemisphere, showing Rheasilvia and Veneneia.
3-D anaglyph image of Rheasilvia's central peak. 3D red cyan glasses are recommended to view this image correctly.

See also

References

  1. ^ a b "Rheasilvia". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.(NASA coordinates)
  2. ^ a b c Vega, Priscilla (11 October 2011). "New View of Vesta Mountain From NASA's Dawn Mission". dawn.jpl.nasa.gov. NASA. Archived from the original on 17 October 2013. Retrieved 17 February 2018.
  3. ^ a b c Schenk, Paul; et al. (11 May 2012). "The Geologically Recent Giant Impact Basins at Vesta's South Pole". Science. 336 (6082): 694–697. Bibcode:2012Sci...336..694S. doi:10.1126/science.1223272. PMID 22582256. S2CID 206541950.
  4. ^ "Hubble Reveals Huge Crater on the Surface of the Asteroid Vesta". HubbleSite. Space Telescope Science Institute. 4 September 1997. Retrieved 4 July 2018.
  5. ^ Drake, Nadia (22 March 2012). "Vesta seems more planet than asteroid". Science News.
  6. ^ Karimi, Saman; Dombard, Andrew J. (2016). "On the possibility of viscoelastic deformation of the large south polar craters and true polar wander on the asteroid Vesta". Journal of Geophysical Research. 121 (9): 1786–1797. Bibcode:2016JGRE..121.1786K. doi:10.1002/2016JE005064.
  7. ^ Thomas, Peter C.; et al. (July 1997). "Vesta: Spin Pole, Size, and Shape from HST Images". Icarus. 128 (1): 88–94. Bibcode:1997Icar..128...88T. doi:10.1006/icar.1997.5736.
  8. ^ Binzel, Richard P.; et al. (1997). "Geologic Mapping of Vesta from 1994 Hubble Space Telescope Images". Icarus. 128 (1): 95–103. Bibcode:1997Icar..128...95B. doi:10.1006/icar.1997.5734.
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