Fig 3
Observations of asteroid 2000 DP107 provided the first images of a binary asteroid in the near-Earth population. Results were published in 2002.
2000 DP107 and 1991 VH made close approaches to Earth in 2008 and provided very good opportunities to characterize the dynamics, morphology, and physical properties of the binary systems. High resolution images obtained over a suitable range of aspect angles provided detailed information on the regolith, size, shape, and spin of the components and on their mutual orbit and dynamical interactions. In conjunction with pre-existing observations, these data probe the formation and evolution of binaries in great detail, including processes such as avalanches, tides, librations, and YORP. Analysis of the 2008 observations is in progress.
Below are some results and animations from our 2000 observations. The 2008 signal-to-noise was 20 times higher, reaching 200 per run for 2000 DP107 and 1500 per run for 1991 VH, and allowed us to obtain higher quality images.
Figures from 2002 Science paper:
|
|
|
A composite of range-Doppler images of binary asteroid 2000 DP107 obtained at Arecibo Observatory 30 Sep-07 Oct 2000. The frame is 5.8 km vertically by 12.2 Hz horizontally, with range, or distance from the observer increasing downward while Doppler, or line-of-sight velocity with respect to the observer, increasing to the right. The resolutions are 75 m in range and 0.24 Hz (15 mm s-1 ) in Doppler. Rotation and revolution are counterclockwise. A roughly spherical primary is visible, as well as a secondary at different phases of the orbital cycle. In this representation the secondary appears much smaller than the primary because its spin rate is lower. The actual size ratio is ~8:3. The orbit appears elliptical in this range-Doppler representation but it is circular in space.
|
|
A schematic diagram representing the sizes of the 2000 DP107 components and their separation, drawn to scale. Click on the image for larger size.
|
|
A schematic diagram representing the sizes of the 2000 DP107 components and their separation, with the Golden Gate bridge for scale. Click on the image for larger size.
|
|
A schematic diagram representing the sizes of the 2000 DP107 components and their separation, with the 320 meter high Eiffel tower for scale. Click on the image for larger size.
|
|
An animation showing the orbital motion of the binary asteroid 2000 DP107 as it would be seen from an observer on Earth close to the time of closest approach on Sep 19, 2000. The animation spans the time interval between Sep 9, 2000 and Oct 9, 2000, so the binary asteroid is first seen to approach then recede. One can see the change in solar illumination as the asteroid travels along its orbit, as well as eclipses and occultations. Also, the orientation of the orbital plane varies as seen by an observer on Earth, because the animation geometry (camera view) changes due to the Earth - asteroid relative motion. Click on the image for the 1.1 MB animation.
|
|
Same as before, except that the distance of the observer is now fixed to better illustrate the eclipses and occultations. Except for distance, the aspect changes due to the relative Earth - asteroid motion are included as above. An eclipse occurs when light from the Sun is obscured. An occultation occurs when one component passes in front of the other as seen by an observer on Earth. Click on the image for the 1.4 MB animation.
|
|
A total eclipse of the primary by the secondary occurs on Sep 30, 2000 near 18:50 UTC. Careful measurements made by Petr Pravec (Ondrejov Observatory, Czech Republic) at the same time showed the brightness attenuation as the secondary obscured light from the sun. Click on the image for a 50 kB animation of the eclipse.
|
Jean-Luc Margot Associate Professor UCLA Earth & Space Sciences and Institute of Geophysics and Planetary Physics 595 Charles Young Drive East Los Angeles, CA 90095 (310) 206 8345
jlm@ess.ucla.edu
Return to my home page.