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Of the expected radio science results at Lutetia are given Read more Impact the probe could be found Moreover some estimates on the accuracy Where not only possible satellites but also small debris that could Restricted three body problem and numerically This characterize the zone Of the orbital stability zone is estimated both in the framework of the The dynamical environment around 21 Lutetia is described The amplitude Is too small to allow a radio science estimate of its mass In this paper
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The body volume derived by the camera measurements an estimate of theĪverage density of the object will be possible On the other hand Steins Tracking residuals This deviation should be comparable to the oneĮxperienced by NEAR while passing by 253 Mathilde and will allow theĭetermination of the mass of the asteroid Together with the estimate of The trajectory of the probe causing a visible signal in the Doppler The second passage in the Main Belt at a distance of about 3000 km withĪ speed of 15 km s The large mass of 21 Lutetia will slightly deviate about 1700 km during itsįirst passage in the Main Belt The Lutetia flyby will take place during Past Steins at about 9 km s at a distance of. Very large diameter 100 km possibly M-type object The probe will fly Reflect the large diversity in the asteroidal population with Steinsīeing a small few km of diameter E-type asteroid and Lutetia being a Past two Main Belt asteroids 2867 Steins and 21 Lutetia These two bodies On its course to the comet 67P Churyumov-Gerasimenko Rosetta will fly Shoulders seen in several lightcurves as the main peak declined are possibly due to material that bounced on first re-entry. A simple ballistic model shows that material ejected toward the limb landed within our direct view at that time. We interpret this as the minimum ejecta flight time before fall back on the atmosphere. The main brightening began ∼6 min after impact for all six of the fragments studied, independent of the location of the impact site behind the limb. Two classes of lightcurves are identified based on the presence of this third precursor emission for the larger G and K impacts and its absence in the lightcurves for smaller fragments. We propose that this may be evidence for continuous ejection of hot material. The emission then faded for the smaller impacts, but slowly increased in strength for the larger G and K impacts in what we identify as a third precursor. This thermal emission was seen as the rising hot plume first came into direct view from Earth. Second precursors were seen ∼1 min after impact for C, D, G, K, and W and lasted for <90 sec. First precursors were seen for the G and K impacts immediately prior to impact, due to thermal emission from the inbound meteor or its trail. Leader emission was seen up to 3.5 min prior to the G and K impacts which we interpret as due to the early impact of cometary coma material that extended along the. We present and discuss 2.34 μm lightcurves and 1-5 μm images for six of these impacts. The CASPIR near-infrared camera was used to record the impacts of fragments C, D, G, K, N, R, V, and W of Comet Shoemaker-Levy 9 with Jupiter.