Bibcode
Meech, K. J.; A'Hearn, M. F.; Adams, J. A.; Bacci, P.; Bai, J.; Barrera, L.; Battelino, M.; Bauer, J. M.; Becklin, E.; Bhatt, B.; Biver, N.; Bockelée-Morvan, D.; Bodewits, D.; Böhnhardt, H.; Boissier, J.; Bonev, B. P.; Borghini, W.; Brucato, J. R.; Bryssinck, E.; Buie, M. W.; Canovas, H.; Castellano, D.; Charnley, S. B.; Chen, W. P.; Chiang, P.; Choi, Y.-J.; Christian, D. J.; Chuang, Y.-L.; Cochran, A. L.; Colom, P.; Combi, M. R.; Coulson, I. M.; Crovisier, J.; Dello Russo, N.; Dennerl, K.; DeWahl, K.; DiSanti, M. A.; Facchini, M.; Farnham, T. L.; Fernández, Y.; Florén, H. G.; Frisk, U.; Fujiyoshi, T.; Furusho, R.; Fuse, T.; Galli, G.; García-Hernández, D. A.; Gersch, A.; Getu, Z.; Gibb, E. L.; Gillon, M.; Guido, E.; Guillermo, R. A.; Hadamcik, E.; Hainaut, O.; Hammel, H. B.; Harker, D. E.; Harmon, J. K.; Harris, W. M.; Hartogh, P.; Hashimoto, M.; Häusler, B.; Herter, T.; Hjalmarson, A.; Holland, S. T.; Honda, M.; Hosseini, S.; Howell, E. S.; Howes, N.; Hsieh, H. H.; Hsiao, H.-Y.; Hutsemékers, D.; Immler, S. M.; Jackson, W. M.; Jeffers, S. V.; Jehin, E.; Jones, T. J.; de Juan Ovelar, M.; Kaluna, H. M.; Karlsson, T.; Kawakita, H.; Keane, J. V.; Keller, L. D.; Kelley, M. S.; Kinoshita, D.; Kiselev, N. N.; Kleyna, J.; Knight, M. M.; Kobayashi, H.; Kobulnicky, H. A.; Kolokolova, L.; Kreiny, M.; Kuan, Y.-J.; Küppers, M.; Lacruz, J. M.; Landsman, W. B.; Lara, L. M.; Lecacheux, A.; Levasseur-Regourd, A. C.; Li, B. et al.
Bibliographical reference
The Astrophysical Journal Letters, Volume 734, Issue 1, article id. L1 (2011).
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6
2011
Citations
103
Refereed citations
91
Description
Earth- and space-based observations provide synergistic information for
space mission encounters by providing data over longer timescales, at
different wavelengths and using techniques that are impossible with an
in situ flyby. We report here such observations in support of the EPOXI
spacecraft flyby of comet 103P/Hartley 2. The nucleus is small and dark,
and exhibited a very rapidly changing rotation period. Prior to the
onset of activity, the period was ~16.4 hr. Starting in 2010 August the
period changed from 16.6 hr to near 19 hr in December. With respect to
dust composition, most volatiles and carbon and nitrogen isotope ratios,
the comet is similar to other Jupiter-family comets. What is unusual is
the dominance of CO2-driven activity near perihelion, which
likely persists out to aphelion. Near perihelion the comet nucleus was
surrounded by a large halo of water-ice grains that contributed
significantly to the total water production.
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