Click on an object in the solar system or choose from the list at left to learn more
|H mag||Request Optical
|2013 WT44||Mar 25-29||High-res Imaging||19.6||Y||Y||BINARY, PHA|
|2009 FD||Mar 29-30||Imaging||22.1||Y||Y||Period = 4.0 or 5.87 h?|
|(363599) 2004 FG11||Apr 07-16||Imaging||21.0||Y||Y||BINARY, period not well known|
|2003 GS||Apr 10-21||Imaging||19.0||Y||Y||NHATS, period unknown|
|(304330) 2006 SX217||Apr 21-24||High-res Imaging||18.8||0.5'||Y||Y||PHA, speckle, period unknown|
|2003 HM||Apr 21-26||Imaging||16.5||20'||Y||PHA, period unknown|
|2013 JX28||Apr 30||Astrometry||20.1||0.5'||Period unknown|
|(387816) 2004 FM17||May 04||Astrometry||19.4||Y||Y||NHATS, period unknown|
|(21374) 1997 WS22||May 07||Astrometry||17.3||Period unknown|
|(242708) 2005 UK1||May 10-28||Imaging||18.0||Y||PHA, period unknown|
|(188174) 2002 JC||May 14-31||Imaging||17.4||Y||Y||2.5-h period|
|2011 JR13||May 18-20||High-res Imaging||19.6||Y||Y||PHA, period unknown|
|2008 WK32||May 18-28||Imaging||19.3||Y||Period unknown|
|2010 UQ7||May 26||Astrometry||20.0||6 deg!||Period unknown|
The Arecibo Planetary Radar discovered that near-Earth Asteroid 2001 SN263 is a triple asteroid system.
The Arecibo Asteroid Dynamics Workshop was held 2003 Feb 2-4 at Arecibo Observatory. Click Here for the workshop web site.
2000 DP107 was the first asteroid identified by radar as a binary system. The primary is roughly spherical with a diameter of 800 meters (a half mile) and the smaller secondary, which orbits it in 1.8 days, is about 300 meters (1000 feet).
The primary has a low density of 1.7 and is assumed to be a "rubble pile" of rocks and voids. It is spinning at a rate near the breakup point for strengthless bodies, and therefore any slight gravitational disturbance can pull it apart. Probably an encounter with the gravity of a planet created the binary by pulling apart the primary.
Four more binary systems have been discovered by radar among the near-Earth asteroids, making one of every 6 a binary.
The illuminated front of a roughly spherical primary is visible, as well as a secondary at different phases of the orbital cycle. In this image the secondary appears much smaller than the primary because its spin rate is lower. The actual size ratio is 8 to 3. Also, the orbit appears elliptical in this image but it is circular in space.
More on 2000 DP107:
Margot web page ,  Klet Observatory optical data ,  IAU Circular #7496 ,  IAU Circular #7503 ,  Table from NeoDys,  Orbit diagram from JPL
Last modified by Alice 23 apr 02