The rotation state of 67P/Churyumov-Gerasimenko from approach observations with the OSIRIS cameras on Rosetta (Articolo in rivista)

Type
Label
  • The rotation state of 67P/Churyumov-Gerasimenko from approach observations with the OSIRIS cameras on Rosetta (Articolo in rivista) (literal)
Anno
  • 2014-01-01T00:00:00+01:00 (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#doi
  • 10.1051/0004-6361/201424590 (literal)
Alternative label
  • S. Mottola, S. Lowry, C. Snodgrass, P.L. Lamy, I. Toth, A. Rozek, A., H. Sierks, M.F. A'Hearn, F. Angrilli, C. Barbieri, M. A. Barucci, J.-L. Bertaux, G. Cremonese, V. Da Deppo, B. Davidsson, M. De Cecco, S. Debei, S. Fornasier, M. Fulle, O. Groussin, P. Gutiérrez, S. F. Hviid, W. Ip, L. Jorda, H. U. Keller, J. Knollenberg, D. Koschny, R. Kramm, E. Kührt, M. Küppers, L. Lara, M. Lazzarin, J. J. Lopez Moreno, F. Marzari, H. Michalik, G. Naletto, H. Rickman, R. Rodrigo, L. Sabau, N. Thomas, K.-P. Wenzel, J. Agarwal, I. Bertini, F. Ferri, C. Güttler, S. Magrin, N. Oklay, C. Tubiana, J.-B. Vincent (2014)
    The rotation state of 67P/Churyumov-Gerasimenko from approach observations with the OSIRIS cameras on Rosetta
    in Astronomy & astrophysics (Print)
    (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#autori
  • S. Mottola, S. Lowry, C. Snodgrass, P.L. Lamy, I. Toth, A. Rozek, A., H. Sierks, M.F. A'Hearn, F. Angrilli, C. Barbieri, M. A. Barucci, J.-L. Bertaux, G. Cremonese, V. Da Deppo, B. Davidsson, M. De Cecco, S. Debei, S. Fornasier, M. Fulle, O. Groussin, P. Gutiérrez, S. F. Hviid, W. Ip, L. Jorda, H. U. Keller, J. Knollenberg, D. Koschny, R. Kramm, E. Kührt, M. Küppers, L. Lara, M. Lazzarin, J. J. Lopez Moreno, F. Marzari, H. Michalik, G. Naletto, H. Rickman, R. Rodrigo, L. Sabau, N. Thomas, K.-P. Wenzel, J. Agarwal, I. Bertini, F. Ferri, C. Güttler, S. Magrin, N. Oklay, C. Tubiana, J.-B. Vincent (literal)
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  • 569 (literal)
Rivista
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  • 5 (literal)
Note
  • Scopu (literal)
  • ISI Web of Science (WOS) (literal)
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  • DLR; University of Kent; Max Planck Society; Centre National de la Recherche Scientifique (CNRS); Hungarian Academy of Sciences; University System of Maryland; University of Padua; PRES University Sorbonne Paris Cite; University of Versailles Saint-Quentin-En-Yvelines; University of Padua; CNR IFN UOS Padova LUXOR; Uppsala University; University of Trento; University of Padua; INAF Osservatorio Astron Trieste; Inst Astrofins Andalucina CSIC; National Central University; Braunschweig University of Technology; European Space Agency; European Space Agency; University of Padua; Inst Datentech & Kommunikat Netze; University of Padua; Consejo Superior de Investigaciones Cientificas (CSIC); Int Space Sci Inst; Inst Nacl Tecn Aeroespacial; University of Bern; University of Padua (literal)
Titolo
  • The rotation state of 67P/Churyumov-Gerasimenko from approach observations with the OSIRIS cameras on Rosetta (literal)
Abstract
  • Aims. Approach observations with the Optical, Spectroscopic, and Infrared Remote Imaging System (OSIRIS) experiment onboard Rosetta are used to determine the rotation period, the direction of the spin axis, and the state of rotation of comet 67P's nucleus. Methods. Photometric time series of 67P have been acquired by OSIRIS since the post wake-up commissioning of the payload in March 2014. Fourier analysis and convex shape inversion methods have been applied to the Rosetta data as well to the available ground-based observations. Results. Evidence is found that the rotation rate of 67P has significantly changed near the time of its 2009 perihelion passage, probably due to sublimation-induced torque. We find that the sidereal rotation periods P1 = 12.76129 ± 0.00005 h and P2 = 12.4043 ± 0.0007 h for the apparitions before and after the 2009 perihelion, respectively, provide the best fit to the observations. No signs of multiple periodicity are found in the light curves down to the noise level, which implies that the comet is presently in a simple rotation state around its axis of largest moment of inertia. We derive a prograde rotation model with spin vector J2000 ecliptic coordinates ? = 65° ± 15°, ? = + 59° ± 15°, corresponding to equatorial coordinates RA = 22°, Dec = + 76°. However, we find that the mirror solution, also prograde, at ? = 275° ± 15°, ? = + 50° ± 15° (or RA = 274°, Dec = + 27°), is also possible at the same confidence level, due to the intrinsic ambiguity of the photometric problem for observations performed close to the ecliptic plane. (literal)
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