EPOXI: Comet 103P/Hartley 2 observations from a worldwide campaign

K. J. Meech, M. F. A'Hearn, J. A. Adams, P. Bacci, J. Bai, L. Barrera, M. Battelino, J. M. Bauer, E. Becklin, B. Bhatt, N. Biver, D. Bockelée-Morvan, D. Bodewits, H. Böhnhardt, J. Boissier, B. P. Bonev, W. Borghini, J. R. Brucato, E. Bryssinck, M. W. BuieH. Canovas, D. Castellano, S. B. Charnley, W. P. Chen, P. Chiang, Y. J. Choi, D. J. Christian, Y. L. Chuang, A. L. Cochran, P. Colom, M. R. Combi, I. M. Coulson, J. Crovisier, N. Dello Russo, K. Dennerl, K. DeWahl, M. A. DiSanti, M. Facchini, T. L. Farnham, Y. Fernández, H. G. Florén, U. Frisk, T. Fujiyoshi, R. Furusho, T. Fuse, G. Galli, D. A. García-Hernández, A. Gersch, Z. Getu, E. L. Gibb, M. Gillon, E. Guido, R. A. Guillermo, E. Hadamcik, O. Hainaut, H. B. Hammel, D. E. Harker, J. K. Harmon, W. M. Harris, P. Hartogh, M. Hashimoto, B. Ḧausler, T. Herter, A. Hjalmarson, S. T. Holland, M. Honda, S. Hosseini, E. S. Howell, N. Howes, H. H. Hsieh, H. Y. Hsiao, D. Hutsemékers, S. M. Immler, W. M. Jackson, S. V. Jeffers, E. Jehin, T. J. Jones, M. De Juan Ovelar, H. M. Kaluna, T. Karlsson, H. Kawakita, J. V. Keane, L. D. Keller, M. S. Kelley, D. Kinoshita, N. N. Kiselev, J. Kleyna, M. M. Knight, H. Kobayashi, H. A. Kobulnicky, L. Kolokolova, M. Kreiny, Y. J. Kuan, M. Küppers, J. M. Lacruz, W. B. Landsman, L. M. Lara, A. Lecacheux, A. C. Levasseur-Regourd, B. Li, J. Licandro, R. Ligustri, Z. Y. Lin, M. Lippi, D. C. Lis, C. M. Lisse, A. J. Lovell, S. C. Lowry, H. Lu, S. Lundin, K. Magee-Sauer, P. Magain, J. Manfroid, E. Mazzotta Epifani, A. McKay, M. D. Melita, H. Mikuz, S. N. Milam, G. Milani, M. Min, R. Moreno, B. E.A. Mueller, M. J. Mumma, M. Nicolini, M. C. Nolan, H. L. Nordh, P. B. Nowajewski, Odin Team, T. Ootsubo, L. Paganini, C. Perrella, J. Pittichová, E. Prosperi, Y. L. Radeva, W. T. Reach, A. J. Remijan, M. Rengel, T. E. Riesen, M. Rodenhuis, D. P. Rodríguez, R. W. Russell, D. K. Sahu, N. H. Samarasinha, A. Sánchez Caso, A. Sandqvist, G. Sarid, M. Sato, D. G. Schleicher, E. W. Schwieterman, A. K. Sen, D. Shenoy, J. C. Shi, Y. Shinnaka, J. Skvarc, C. Snodgrass, M. L. Sitko, S. Sonnett, S. Sosseini, G. Sostero, S. Sugita, B. M. Swinyard, S. Szutowicz, N. Takato, P. Tanga, P. A. Taylor, G. P. Tozzi, R. Trabatti, J. M. Trigo-Rodríguez, C. Tubiana, M. De Val-Borro, W. Vacca, B. Vandenbussche, J. Vaubaillion, F. P. Velichko, S. F. Velichko, R. J. Vervack, M. J. Vidal-Nunez, G. L. Villanueva, C. Vinante, J. B. Vincent, M. Wang, L. H. Wasserman, J. Watanabe, H. A. Weaver, P. R. Weissman, S. Wolk, D. H. Wooden, C. E. Woodward, M. Yamaguchi, T. Yamashita, P. A. Yanamandra-Fischer, B. Yang, J. S. Yao, D. K. Yeomans, T. Zenn, H. Zhao, J. E. Ziffer

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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 16.4hr. Starting in 2010 August the period changed from 16.6hr to near 19hr 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 CO 2 -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.

Original languageEnglish
Article numberL1
JournalAstrophysical Journal Letters
Issue number1
StatePublished - 10 Jun 2011


  • comets: individual (103P/Hartley 2)


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