Richard Nugent's Asteroid Occultation Basics....
Asteroid Occultations
Stellar Eclipses by Asteroids
Asteroid Occultation Video - 10 second MPEG video clip of 1587 Kahrstedt on 10-20-4. 1.8 Meg size.
UPCOMING EVENTS:
940 Kordula occults a m=11.3 star over Houston Thursday evening October 11, 2007 at 10:43 pm CDT.
See asteroid profiles from recent occultations here
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Asteroid Occultation Basics
1. What is an asteroid occultation?
2. Why observe asteroid occultations?
3. How is the asteroid size/shape determined from the occultation ?
4. What equipment is best to record an asteroid occultation? Video setup Visual setup
5. Problems in observing asteroid occultations Weather conditions Equipment problems Path shifts Local surprises
6. How to find out about the next occultation over your area
7. How to report an asteroid occultation observation
ASTEROID OCCULTATION TOPICS:
1. What is an Asteroid Occultation ?
An "asteroid occultation" occurs when an asteroid, while moving in its orbit around the Sun, passes in front of ("occults") a relatively bright star as seen from Earth. An "occultation" is a technical term to describe a certain type of eclipse. See the diagram below as Figure 1 to see how an asteroid occultation occurs.
2. Why observe Asteroid Occultations ?
The exciting field of asteroid occultations is wide open for both amateurs and professionals alike. Observing these occultations are the only direct method to determine the size and shape of these mysterious objects. IOTA astronomers were the first to discover asteroid moons by this technique, indicated by a 2nd occultation as the asteroid moon drifts in front of the target star.
Figure 1. Geometry of an asteroid occultation
3. How is the asteroid size/shape determined from the occultation?
In the above Figure 1, observers are lined up in the path (shadow) of the asteroid on the Earth. The shadow is caused by the asteroid blocking out the star's light. Note that the diagram is not to scale. As the asteroid moves in its orbit, each observer that is in the path of the asteroid's shadow, will see the star vanish. The duration of time that the star vanishes is usually less than one second (near the edge of the shadow) to several seconds near to the center. Since the star vanishes for several seconds as the dark asteroid moves in front of it, its size and shape can be determined from analysis of their observations and their exact location on the ground.
In the diagram below, Observers 1-6 will see an occultation. Also note that Observer # 1 will see the occultation at a different time than Observer # 6, caused by the orientation angle of the asteroid. Observer # 7 will not see an occultation, thus he has a "miss". Even Observer # 7 who does not see the occultation as the asteroid glides in front of the star, can offer valuable data as his observation is used to place a limitation on that side for the size of the asteroid. Keep in mind a "miss" observation has nothing to do with clouds or other factors preventing an observer from seeing the target star. A "miss" is when the observer watches the target star and does not see the occultation.
An example of how the observations are computed to determine a size and shape of an asteroid is shown in the figure below of the occultation of the Star TYC 7902:1828 by the asteroid 54 Alexandra. In the diagram, David Dunham (chord #11) in San Bartolo, Mexico and Art Lucas (chord #12) in Stillwater, OK had miss observations near to the northern and southern side of the asteroid while the other observers did have occultations of different durations.
A 'miss' observation simply means that the observer did not see the star get occulted (covered up) by the asteroid. But a 'miss' observation is very critical in determining the size limits of the asteroid. 54 Alexandra's occultation proved to be a long one, as Nugent had an occultation that was 63 seconds in duration.
Peter Armstrong (chord #1 at the northern limit), from Limpia Observatory in Ft. Davis, Texas, observed a brief occultation of just 0.9 second placing him a the very northern edge of the asteroid. Rebecca Alestick (chord #12) observing in Guthrie OK, was very near the asteroid's southern limit and recorded a 9-second occultation.
The "ellipse" surrounding the numbered chords represents the asteroids average size shape. The observers do not need to be in a straight line perpendicular to the asteroid's shadow path; the computer program compensates for this in the final analysis. Thus from the successful observation of this asteroid, IOTA astronomers have estimated the size of the asteroid 54 Alexandra as 159.9 x 132.4 kilometers. This size is accurate to less than 2%. (1 kilometer = 0.6 miles)
The occultation of a magnitude m = +5.4 star by the asteroid 828 Lindemannia was observed by 12 observers in the Houston and San Antonio areas and its resulting size/shape profile is indicated below:
Lindemannia's average size came to 50 x 52 km. Again, one can see that the observer represented by chord 12 (Becky Ramotowski) at the lower portion of the plot had a miss. This chord is plotted for reference. Note that the ellipse plotted does not perfectly intersect all of the observers start and end times of the occultation, rather it represents an "average" fit for all the observations. This is mainly due to errors in the actual derived times from visual observations. This error is called "personal equation" or "reaction time". These reaction times are the result of a delay in the recording an occultation by voice following actually seeing the occultation, and averages 0.3 - 0.75 seconds and longer. Even when these reaction times are applied to the raw observations, the ellipse will not fit perfectly, after all, asteroids are usually irregular chunks of rock. Reaction times can be eliminated by using a video system to record the occultation. The video tapes can be analyzed frame by frame and accuracies of 0.03 second can be achieved.
IOTA astronomers are actively seeking observers for asteroid occultations. The main IOTA web page includes useful information on lunar and asteroid occultations. |
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This site was last updated 02/08/08