Durech, J., Vokrouhlický, D., Kaasalainen, M., Weissman, P., Lowry, S.C., Beshore, E., Higgins, D., Krugly, Y.N., Shevchenko, V.G., Gaftonyuk, N.M., and others. (2008) New photometric observations of asteroids (1862) Apollo and (25143) Itokawa - An analysis of YORP effect. Astronomy and Astrophysics, 488 (1). pp. 345-350. ISSN 0004-6361. E-ISSN 1432-0746. (doi:10.1051/0004-6361:200809663) (The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided) (KAR id:52296)
| The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided. | |
| Official URL: http://dx.doi.org/10.1051/0004-6361:200809663 |
Abstract
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 , 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 to . This is inconsistent with results of lightcurve inversion that place an upper limit to the change of Itokawa's rotation rate . . © 2008 ESO.
| Item Type: | Article |
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| DOI/Identification number: | 10.1051/0004-6361:200809663 |
| Additional information: | Unmapped bibliographic data: LA - English [Field not mapped to EPrints] J2 - Astron. Astrophys. [Field not mapped to EPrints] AD - Astronomical Institute, Charles University in Prague, V HolÄ?oviÄ?kách 2, 18000 Prague, Czech Republic [Field not mapped to EPrints] AD - Department of Mathematics and Statistics, Rolf Nevanlinna Institute, University of Helsinki, PO Box 68, 00014 Helsinki, Finland [Field not mapped to EPrints] AD - Science Division, Jet Propulsion Laboratory, MS 183-301, 4800 Oak Grove Drive, Pasadena, CA 91109, United States [Field not mapped to EPrints] AD - Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721-0092, United States [Field not mapped to EPrints] AD - Hunters Hill Observatory, 7 Mawalan Street, Ngunnawal, ACT 2913, Australia [Field not mapped to EPrints] AD - Institute of Astronomy, Kharkiv National University, Sumska str. 35, Kharkiv, 61022, Ukraine [Field not mapped to EPrints] AD - Crimean Astrophysical Observatory, Simeiz, 98680, Ukraine [Field not mapped to EPrints] AD - Korea Astronomy and Space Science Institute, 61-1 Hwa-am Dong, Yuseong Gu, Daejon, 305-348, South Korea [Field not mapped to EPrints] AD - Palmer Divide Observatory, Colorado Springs, CO 80908, United States [Field not mapped to EPrints] AD - Ulugh Beg Astronomical Institute, Uzbek Academy of Sciences, Astronomicheskaya 33, Tashkent, 100052, Uzbekistan [Field not mapped to EPrints] AD - Keldysh Institute of Applied Mathematics, RAS, Miusskaya sq. 4, Moscow, 125047, Russian Federation [Field not mapped to EPrints] AD - Astronomical Observatory, Adam Mickiewicz University, SÅ?oneczna 36, 60-286 PoznaÅ?, Poland [Field not mapped to EPrints] AD - Department of Earth and Planetary Science, University of Tokyo, Bynkyo-ku, Tokyo, 113-0033, Japan [Field not mapped to EPrints] DB - Scopus [Field not mapped to EPrints] |
| Uncontrolled keywords: | Methods: data analysis, Minor planets, asteroids, Techniques: photometric, Forecasting, Metal working shapers, Photometry, Rotation, Spin dynamics, Free parameters, High degree of accuracy, Inversion methods, Itokawa, Methods: data analysis, Minor planets, asteroids, New model, Rotation periods, Rotation rates, Shape Modelling, Spin states, Techniques: photometric, Time-line, Upper limits, Asteroids |
| Subjects: | Q Science > QB Astronomy |
| Divisions: | Divisions > Division of Natural Sciences > Physics and Astronomy |
| Depositing User: | Stephen Lowry |
| Date Deposited: | 08 Dec 2015 22:46 UTC |
| Last Modified: | 05 Nov 2024 10:38 UTC |
| Resource URI: | https://kar.kent.ac.uk/id/eprint/52296 (The current URI for this page, for reference purposes) |
University of Kent Author Information
Lowry, S.C..
| Creator's ORCID: |
 https://orcid.org/0000-0002-5605-4329
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