EDP Sciences
Free Access
Volume 488, Number 1, September II 2008
Page(s) 345 - 350
Section Planets and planetary systems
DOI https://doi.org/10.1051/0004-6361:200809663
Published online 16 June 2008

A&A 488, 345-350 (2008)
DOI: 10.1051/0004-6361:200809663

New photometric observations of asteroids (1862) Apollo and (25143) Itokawa - an analysis of YORP effect

J. Durech1, D. Vokrouhlický1, M. Kaasalainen2, P. Weissman3, S. C. Lowry3, E. Beshore4, D. Higgins5, Y. N. Krugly6, V. G. Shevchenko6, N. M. Gaftonyuk7, Y.-J. Choi3, 8, R. A. Kowalski4, S. Larson4, B. D. Warner9, A. L. Marshalkina10, M. A. Ibrahimov10, I. E. Molotov11, T. Michalowski12, and K. Kitazato13

1  Astronomical Institute, Charles University in Prague, V Holesovickách 2, 18000 Prague, Czech Republic
    e-mail: durech@sirrah.troja.mff.cuni.cz
2  Department of Mathematics and Statistics, Rolf Nevanlinna Institute, PO Box 68, 00014 University of Helsinki, Finland
3  Science Division, Jet Propulsion Laboratory, 4800 Oak Grove Drive, MS 183-301, Pasadena, CA 91109, USA
4  Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721-0092, USA
5  Hunters Hill Observatory, 7 Mawalan Street, Ngunnawal ACT 2913, Australia
6  Institute of Astronomy of Kharkiv National University, Sumska str. 35, Kharkiv 61022, Ukraine
7  Crimean Astrophysical Observatory, Simeiz 98680, Ukraine
8  Korea Astronomy & Space Science Institute, 61-1 Hwa-am Dong, Yuseong Gu, Daejon 305-348, South Korea
9  Palmer Divide Observatory, Colorado Springs, Colorado 80908, USA
10  Ulugh Beg Astronomical Institute, Uzbek Academy of Sciences, Astronomicheskaya 33, Tashkent 100052, Uzbekistan
11  Keldysh Institute of Applied Mathematics, RAS, Miusskaya sq. 4, Moscow 125047, Russia
12  Astronomical Observatory, Adam Mickiewicz University, Sloneczna 36, 60-286 Poznan, Poland
13  Department of Earth and Planetary Science, The University of Tokyo, Bynkyo-ku, Tokyo 113-0033, Japan

Received 27 February 2008 / Accepted 18 May 2008

Aims. Asteroid (1862) Apollo is one of two asteroids in which the YORP effect was detected. We carried out new photometric observations of Apollo in April 2007 to enlarge the time line and to derive a more precise shape and spin state model. We also observed another YORP-candidate, asteroid (25143) Itokawa, in December 2006 and January 2007 to obtain a longer time line. An estimation of the YORP strength on Itokawa based on its precise shape model from the Hayabusa mission predicted the deceleration to be already observable during the 2007 apparition.
Methods. We used the lightcurve inversion method to model the shape and spin state of Apollo. For Itokawa, the shape and pole direction are known to a high degree of accuracy from the Hayabusa mission, so we used a modified version of lightcurve inversion with only two free parameters - the rotation period and its linear change in time.
Results. The new model of Apollo confirms earlier results. The observed acceleration of Apollo's rotation rate is $(5.5 \pm 1.2) \times 10^{-8}\,\mathrm{rad\,d}^{-2}$, which is in agreement with the theoretically predicted value. For Itokawa, the theoretical YORP value is sensitive to the resolution of the shape model and lies in the range from -2 to $-3\times 10^{-7}\,\mathrm{rad\,d}^{-2}$. This is inconsistent with results of lightcurve inversion that place an upper limit to the change of Itokawa's rotation rate $\sim $ $1.5 \times 10^{-7}\,\mathrm{rad}\,\mathrm{d}^{-2}$.

Key words: minor planets, asteroids -- methods: data analysis -- techniques: photometric

© ESO 2008

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