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By Stebbins J.

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Extra resources for Absorption and Space Reddening in the Galaxy as Shown by the Colors of Globular Clusters

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The most important improvement needed was to make the orbit solutions consistent with the observed impact times. If the solutions could be updated to "predict" the correct impact times, estimates of other parameters such as the impact locations would also become more accurate. Although this update could have been accomplished by making the impact time a constraint and forcing the orbit solution to satisfy it exactly, a betterapproach was simply to use the impact time as an additional measurement in the solution process.

Geophys. Res. Lett. 22, 1561. CHODAS, P. W. 1993 Estimating the impact probability of a minor planet with the earth. Bull. Am. Astron. Soc. 25, 1236. CHODAS, P. , Sz YEOMANS, D. K. 1993 The upcoming collision of comet Shoemaker-Levy 9 with Jupiter. Bull. Am. Astron. Soc. 25, 1042. CHODAS, P. , Sz YEOMANS, D. K. 1994a The impact of comet Shoemaker-Levy 9 with Jupiter. Bull. Am. Astron. Soc. 26, 1022. CHODAS, P. , Sz YEOMANS, D. K. 1994b Comet Shoemaker-Levy 9 impact times and impact geometries. Bull.

K. 003294 Mar. 990216 Mar. 981965 Mar. 972968 Mar. 966629 Mar. 948463 Mar. 935514 Mar. 912868 Mar. 885070 Mar. 863131 Mar. 840458 Mar. 831257 Mar. 829288 Mar. 823607 Mar. 822819 Mar. 805868 Mar. 788483 Mar. 783002 Mar. 776310 Mar. 764890 Apr. 758370 Apr. 63988 TABLE 3. 5 TDB. '), and time of perihelion passage (Tp). The angular orbital elements are referred to the ecliptic plane and equinox of J2000. A B C D E F G H K L N P2 PI Q2 Ql R S T U with a scatter much smaller than the bias. We concluded that the bias was mostly due to star catalog errors, while the scatter was mostly due to the actual errors of measurement.

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