Valhalla (crater)

Valhalla multiring structure on Callisto

Valhalla is the largest multi-ring structure (impact crater) on Jupiter's moon Callisto and in the Solar System. It was named after Valhalla, Odin's hall in Norse mythology. Valhalla consists of a bright central region 360 km across, an inner ridge and trough zone and striking concentric rings extending up to about 1,900 km from the center.^[1] Several large impact craters and catenae are superimposed on Valhalla. Valhalla multi-ring system is of impact origin and may have formed as semi-liquid or liquid material underlying the brittle lithosphere punctured by the impactor slumped towards the center of the crater following the impact.^[2]

General description

Valhalla is the largest multi-ring basin on Callisto and in the Solar System (with diameter up to 3,800 km).^[3] It was discovered by the Voyager probes in 1979–80 and is located in the leading hemisphere of Callisto, in its Jupiter facing quadrant slightly to the north of the equator (at about 18°N latitude and 57°W longitude). From the geological point of view Valhalla consists of three zones: A central zone, an inner ridge-and-trough zone, and an outer trough zone.

The central part of Valhalla structure on Callisto. Bright knobs surrounded by smooth dark plains are visible.

The inner zone (diameter of about 360 km) is an example of a palimpsest: a high albedo circular feature of the impact origin. The surface in the central zone is relatively smooth and has a mottled appearance. Many impact craters inside it have dark halos. At the high resolution achieved in some Galileo images the central part of Valhalla looks like a knobby terrain, where bright knobs are surrounded by dark smooth plains; there is noticeable deficit of small impact craters.^[1]

The inner ridge and trough zone surrounds the central palimpsest. The ridges that immediately surround the central zone have steep flanks facing outward. These scarps, when studied at high resolution, turned out to be discontinuous consisting of a series of small bright knobs surrounded by the smooth dark material. They are obviously very degraded structures. The troughs that are situated further from the center than ridges are sinuous and appear to be grabens (about 20 km wide). The inner trough zone extends up to 950 km from the center of Valhalla.^[1]

The outer trough zone has the radius of 1500–1900 km; its outer boundary is not well defined. It consists of wide double walled sinuous lineaments (troughs), which like inner troughs appear to be grabens. Though these grabens are wider (up to 30 km) than those in the inner trough zone, they are severely degraded, and consist of a series of small knobs, much like their inner counterparts. There are no indications of volcanic flows or other signs of endogenic activity associated with the grabens on high resolution Galileo images as was suggested based on Voyager data. All structures within Valhalla basin have impact or tectonic origin.^[1]

Craters

Several prominent impact craters and catenae are located with Valhalla structure. At the northern margin of it, Gomul Catena can be found as well as Egdir and Mimir craters. The catena consists of a linear sequence of impact craters and probably resulted from a break-up of a comet (like comet Shoemaker-Levy 9).^[1] To the south of Valhalla there are Sarakka and Nar impact craters; to the east of it (at the boundary between the inner and outer trough zones) are Sculd crater and Svol Catena. To the west of Valhalla another large multi-ring basin—Asgard—can be found.^[4] The central parts of Valhalla are less cratered than the old plain outside the structure. This indicates that Valhalla is significantly younger than Callisto itself.^[1]

Origin

The troughs (faults) surrounding Valhalla

The Valhalla multi-ring structure (like other Callistan multi-ring basins) probably resulted from a giant impact, which punctured the outer ridged lithosphere of the moon and entered the underlying layer consisting of a much softer material.^[5] The latter can be warm ice or even a liquid ocean, which existence was implied from the magnetometric data.^[6] The formation of a ringed structure is caused by the concentric failure of the brittle outer shell (lithosphere) following the impact, after the soft material underlying the lithosphere flows towards the center to fill the cavity excavated by the impact.^[2] The absolute age of the Valhalla structure is not known; however, it is the youngest such feature among the five known multi-ring structures on Callisto. Estimates of its age vary from 2 to 4 billion years.^[1]

Consistent with this picture, imaging by the Galileo spacecraft found no evidence of disruption of the area of Callisto antipodal to Valhalla. Such disrupted terrain normally forms as a result of focusing of the seismic energy at the opposite point after the impact. The absence of such disruption supports the presence of a subsurface ocean, which would have absorbed much of the seismic energy, at the time of Valhalla's formation.^[7]

See also

• Adlinda (crater)
• List of geological features on Callisto

References

1. ^ ^{a b c d e f g} Greeley, R.; Klemaszewski, J.E.;Wagner L.; et al. (2000). "Galileo views of the geology of Callisto". Planetary and Space Science 48 (9): 829–853. Bibcode 2000P&SS...48..829G. doi:10.1016/S0032-0633(00)00050-7. 
2. ^ ^{a b} Shenk, Paul M. (1995). "The geology of Callisto". Journal of Geophysical Research 100 (E9): 19,023–40. Bibcode 1995JGR...10019023S. doi:10.1029/95JE01855. 
3. ^ "Callisto, one of Jupiter’s moons, 1979". Science & Society. http://www.scienceandsociety.co.uk/results.asp?image=10299355. Retrieved February 5, 2009. 
4. ^ U.S. Geological Survey. Controlled Photomosaic Map of Callisto JC 15M CMN (Map) (2002 ed.). http://astrogeology.usgs.gov/Gallery/MapsAndGlobes/joviansatellites.html. 
5. ^ Klemaszewski, J.A.; Greeley, R. (2001). "Geological Evidence for an Ocean on Callisto" (pdf). Lunar and Planetary Science XXXI. pp. 1818. http://www.lpi.usra.edu/meetings/lpsc2001/pdf/1818.pdf. 
6. ^ Spohn, T.; Schubert, G. (2003). "Oceans in the icy Galilean satellites of Jupiter?" (pdf). Icarus 161 (2): 456–467. Bibcode 2003Icar..161..456S. doi:10.1016/S0019-1035(02)00048-9. http://lasp.colorado.edu/icymoons/europaclass/Spohn_Schubert_oceans.pdf. 
7. ^ Moore, Jeffrey M.; Chapman, Clark R.; Bierhaus, Edward B. et al. (2004). "Callisto". In Bagenal, F.; Dowling, T.E.; McKinnon, W.B. (pdf). Jupiter: The planet, Satellites and Magnetosphere. Cambridge University Press. http://lasp.colorado.edu/~espoclass/homework/5830_2008_homework/Ch17.pdf.