Click on an object in the solar system or choose from the list at left to learn more
|H mag||Request Optical
|(276049) 2002 CE26||Aug 26-05||High-res Imaging||16.8||Y||Y||BINARY, 3.3-h period, C type|
|(299582) 2006 GQ2||Sep 25||Astrometry||18.0||Period unknown|
|2009 FG19||Sep 25-26||Imaging||17.9||Y||PHA, period unknown|
|2008 OB9||Oct 02||Astrometry||17.5||PHA, period unknown|
|2012 TS||Oct 03||Astrometry||20.8||Period unknown|
|(68267) 2001 EA16||Oct 11-14||Imaging||16.8||Y||Period unknown|
|2340 Hathor||Oct 14-30||High-res Imaging||20.0||Y||Y||PHA, period unknown, Sq type|
|2012 KY3||Oct 20||Astrometry||18.6||PHA, period unknown|
|(36017) 1999 ND43||Oct 30||Astrometry||19.1||11.4-h period, Sl type|
|(163818) 2003 RX7||Nov 07||Astrometry||18.4||PHA, 2.6-h period|
|(85713) 1998 SS49||Nov 21||Astrometry||15.6||PHA, period unknown|
|(393908) 2005 UH3||Nov 23-30||Imaging||16.4||Y||Period unknown|
|(214088) 2004 JN13||Dec 03-12||Imaging||15.0||Y||Period unknown|
|(345705) 2006 VB14||Dec 12||Astrometry||18.5||3.25-h period|
|(204131) 2003 YL||Dec 04-23||Imaging||19.8||Y||Period unknown|
|2001 XY10||Dec 21||Astrometry||19.1||Period unknown, Sk class|
|2005 YQ96||Dec 26-31||High-res Imaging||20.4||Y||Y||PHA, period unknown|
|2007 EC||Jan 06||Astrometry||16.4||2 deg!||NHATS, period unknown|
|2007 EJ||Jan 07||Astrometry||18.1||Period unknown|
|(357439) 2004 BL86||Jan 27||High-res Imaging||18.9||4'||Y||Y||PHA, 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