## Click on an object in the solar system or choose from the list at left to learn more |

(363599) 2004 FG11

2014 GP17

2014 GO17

2009 FD

(143469) 2003 QQ47

2013 WT44 - Found to be a binary system by Goldstone!

2014 FO38

2014 EQ12

2014 EY24 - Line-of-sight range correction of almost one Earth radius!

2014 AY28

2014 EL45 - Line-of-sight range correction of almost one Earth diameter!

(357622) 2005 EY95

(275677) 2000 RS11 - Very oddly shaped contact binary much like Mithra!

2014 DJ23

2014 AD16

2013 YZ13

2062 Aten - Detected for the third time in 3 years

2010 XZ67 - First detected in Dec 2013

Asteroid | Dates | Expected Results |
IRTF Target? |
H mag | Request Optical Astrometry? |
Request Optical Lightcurve? |
Request Optical Characterization? |
Notes |

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 |

99942 Apophis

2013 CZ87

2008 DG17

785 Zwetana

2013 EC20

1993 UC - Found to be a binary system!

14 Irene

2009 SC15

2013 EA

2008 SE85

2001 TA2

29 Amphitrite

2013 FY13

2013 GJ69

(232643) 2005 NZ6

2013 GR38

(360191) 1988 TA

2010 VA1

(137199) 1999 KX4

(152756) 1999 JV3

(163249) 2002 GT - Would have been the target of a Deep Impact flyby (RIP)

2013 JB36

(285263) 1998 QE2 - Found to be a binary system (first detected by Goldstone)!

2004 KH17

2013 LB2 - Line-of-sight range correction of almost 2 Earth radii!

2013 JR28

2013 LL25

1627 Ivar

2013 LC7

(340666) 2006 RO36

(17188) 1999 WC2

(363790) 2005 JE46

2062 Aten

(153349) 2001 PJ9

(7753) 1988 XB

2003 DZ15

(277475) 2005 WK4

2013 QR1

2013 PR43

2009 WH106

2010 CF19

2007 CN26

(52760) 1998 ML14

(232691) 2004 AR1

(363305) 2002 NV16

329 Bamberga

2013 HG20

(329437) 2002 OA22

89 Julia

(152664) 1998 FW4

2013 QN11

(24445) 2000 PM8

2013 RH74

6063 Jason

712 Boliviana

2013 VO5

2013 VJ11

2011 JY1

216 Kleopatra

572 Rebekka

161 Athor

(138095) 2000 DK79 - Found to be a binary system!

1997 WQ23

(85774) 1998 UT18

2013 UF3

2001 AV43

2010 CL19

64 Angelina

2009 WZ104

2006 CT

2013 XZ9

2013 XY8

2013 XA4

2013 NJ

2013 XG10

2013 XH22

2013 XX8

2010 XZ67

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