Goldstone Solar System Radar

Summary

Goldstone Solar System Radar
Goldstone Deep Space Network.jpg
Goldstone Deep Space Network
Alternative namesGSSR Edit this at Wikidata
Part ofDSS 14 Edit this on Wikidata
Location(s)California
Coordinates35°25′36″N 116°53′24″W / 35.4267°N 116.89°W / 35.4267; -116.89Coordinates: 35°25′36″N 116°53′24″W / 35.4267°N 116.89°W / 35.4267; -116.89 Edit this at Wikidata
OrganizationCalifornia Institute of Technology
Jet Propulsion Laboratory
NASA Edit this on Wikidata
Altitude2,950 ft (900 m) Edit this at Wikidata
Telescope styleradar
radio telescope
space instrument Edit this on Wikidata
Diameter70 m (229 ft 8 in) Edit this at Wikidata
Websitegssr.jpl.nasa.gov Edit this at Wikidata
Goldstone Solar System Radar is located in the United States
Goldstone Solar System Radar
Location of Goldstone Solar System Radar

The Goldstone Solar System Radar (GSSR) is a large radar system used for investigating objects in the Solar System. Located in the desert near Barstow, California, it comprises a 500-kW X-band (8500 MHz) transmitter and a low-noise receiver on the 70-m DSS 14 antenna at the Goldstone Deep Space Communications Complex. It has been used to investigate Mercury, Venus, Mars, the asteroids, and moons of Jupiter and Saturn. The most comparable facility was the radar at Arecibo Observatory,[1] until that facility collapsed. GSSR now stands alone.

Planetary observations

GSSR can work in two different modes. In the monostatic radar mode, GSSR both transmits and receives. In bistatic mode, GSSR transmits and other radio astronomy facilities receive. Although more difficult to schedule, this offers two advantages - the transmitter does not need to turn off to allow the receiver to listen, and it allows the use of interferometry to extract more information from the reflected signal.

Bodies that have been investigated using GSSR include:

  • Mercury: In particular, by watching specific reflected features of Mercury sweep across the Earth's surface (using spatially separated receivers), GSSR enables the pole position to be computed quite accurately. The measured librations show Mercury has a liquid core.
  • Venus[2]
  • Mars: GSSR was used extensively to characterize sites for Mars landers.
  • Asteroids: Asteroids appear only as unresolved points of light in ground-based optical telescopes. Radar, however, can image near-Earth asteroids and comets with a resolution of several meters. For example, the asteroid 4179 Toutatis was imaged in 1992, 1996, 2000, 2004, 2008, and 2012. Although spacecraft such as Dawn can image particular asteroids in much finer detail, radar astronomy can investigate many more asteroids of different characteristics. For example, all existing images of binary asteroids were obtained through radar astronomy.[3][4]
  • Moons of Jupiter
  • Rings and moons of Saturn

Other scientific uses

References

  1. ^ Slade, Martin, Lance AM Benner, and Arnold Silva (2011). "Goldstone solar system radar observatory: Earth-based planetary mission support and unique science results" (PDF). Proceedings of the IEEE. 99 (5): 757–769. doi:10.1109/jproc.2010.2081650.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  2. ^ Williams, Matt (4 May 2021). "How Long is a Day on Venus? We Finally Know the Exact Answer". Universe Today. Universe Today.
  3. ^ Brozović, Marina; Benner, Lance A. M.; Giorgini, Jon D.; Naidu, Shantanu P.; Busch, Michael W.; Lawrence, Kenneth J.; Jao, Joseph S.; Lee, Clement G.; Snedeker, Lawrence G.; Silva, Marc A.; Slade, Martin A.; Chodas, Paul W. (27 December 2018). "Goldstone Radar Observations of Horseshoe-orbiting Near-Earth Asteroid 2013 BS45, a Potential Mission Target". The Astronomical Journal. 157 (1): 24. doi:10.3847/1538-3881/aaf04f.
  4. ^ Lawrence, Kenneth J.; Benner, Lance A.M.; Brozovic, Marina; Ostro, Steven J.; Jao, Joseph S.; Giorgini, Jon D.; Slade, Martin A.; Jurgens, Raymond F.; Nolan, Michael C.; Howell, Ellen S.; Taylor, Patrick A. (January 2018). "Arecibo and Goldstone radar images of near-Earth Asteroid (469896) 2005 WC1". Icarus. 300: 12–20. doi:10.1016/j.icarus.2017.08.028.