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| 題名: | The rotation state of 67P/Churyumov-Gerasimenko from approach observations with the OSIRIS cameras on Rosetta |
| 作者: | 葉永烜;Mottola, S.;Lowry, S.;Snodgrass, C.;Lamy, P. L.;Toth, I.;Rożek, A.;Sierks, H.;A’Hearn, M. F.;Angrilli, F.;Barbieri, C.;Barucci, M. A.;Bertaux, J.-L.;Cremonese, G.;Da Deppo, V.;Davidsson, B.;De Cecco, M.;Debei, S.;Fornasier, S.;Fulle, M.;Groussin, O.;Gutiérrez, P.;Hviid, S. F.;Ip, W.;Jorda, L.;Keller, H. U.;Knollenberg, J.;Koschny, D.;Kramm, R.;Kührt, E.;Küppers, M.;Lara, L.;Lazzarin, M.;Lopez Moreno, J. J.;Marzari, F.;Michalik, H.;Naletto, G.;Rickman, H.;Rodrigo, R.;Sabau, L.;Thomas, N.;Wenzel, K.-P.;Agarwal, J.;Bertini, I.;Ferri, F.;Güttler, C.;Magrin, S.;Oklay, N.;Tubiana, C.;Vincent, J.-B. |
| 貢獻者: | 理學院天文研究所 |
| 關鍵詞: | Astrophysics;Comet nuclei;Comets;comets: general;comets: individual: 67P/Churyumov-Gerasimenko;Confidence intervals;Ecliptic;Ground-based observation;Mathematical models;Perihelions;Photometry;Sciences of the Universe;techniques: photometric |
| 日期: | 2014-01-01 |
| 上傳時間: | 2026-04-21 14:25:04 (UTC+8) |
| 出版者: | EDP Sciences |
| 摘要: | 摘要： 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 λ = 65° ± 15°, β = + 59° ± 15°, corresponding to equatorial coordinates RA = 22°, Dec = + 76°. However, we find that the mirror solution, also prograde, at λ = 275° ± 15°, β = + 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.
出版者： EDP Sciences
出版日期： 2014-09-01
出處： Astronomy and astrophysics (Berlin), 2014-09, Vol.569, p.L2-5
資源來源： EDP Sciences
版權： CC0 1.0 - Universal
識別號： ISSN: 0004-6361
識別號： ISSN: 1432-0746
識別號： EISSN: 1432-0746
識別號： DOI: 10.1051/0004-6361/201424590 |
| 顯示於類別: | [天文研究所] 期刊論文
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