EDP Sciences
Free Access
Volume 405, Number 3, July III 2003
Page(s) L29 - L32
Section Letters
DOI https://doi.org/10.1051/0004-6361:20030819

A&A 405, L29-L32 (2003)
DOI: 10.1051/0004-6361:20030819


CCD photometry and model of MUSES-C target (25143) 1998 SF36

M. Kaasalainen1, T. Kwiatkowski2, M. Abe3, J. Piironen1, T. Nakamura4, Y. Ohba3, B. Dermawan5, T. Farnham6, F. Colas7, S. Lowry8, P. Weissman8, R. J. Whiteley9, D. J. Tholen10, S. M. Larson9, M. Yoshikawa3, I. Toth11 and F. P. Velichko12

1  Observatory, University of Helsinki, PO Box 14, 00014 Helsinki, Finland
2  Astronomical Observatory, Adam Mickiewicz University, ul. Sloneczna 36, 60-286 Poznan, Poland
3  The Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
4  National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan
5  School of Science, The University of Tokyo, Bynkyo, Tokyo 113-0033, Japan
6  Department of Astronomy, University of Texas at Austin, Austin, TX 78712, USA
7  IMCCE, Observatoire de Paris, 77 Av. Denfert Rochereau, 75014 Paris, France
8  Earth and Space Sciences Division, Jet Propulsion Laboratory, Pasadena, CA 91109, USA
9  Lunar and Planetary Laboratory, University of Arizona, 1629 E. Univ. Blvd. Tucson, AZ 85721-0092, USA
10  Institute for Astronomy, Woodlawn Drive, 96822, Honolulu, HI, USA
11  Konkoly Observatory, Post Office Box 67, Budapest 1525, Hungary
12  Astronomical Observatory of Kharkiv National University, 35 Sums'ka St., 61022 Kharkiv, Ukraine

(Received 5 May 2003 / Accepted 31 May 2003)

We present photometric observations of the near-Earth asteroid (25143) 1998 SF36 from the 2001 apparition campaign, and we discuss the corresponding physical model. The asteroid's photometric behaviour is consistent with an S-type object, it has a retrograde pole at $\lambda=355^\circ,\ \ \beta=-84^\circ\pm 5^\circ$, and its sidereal rotation period is $P=12.132\pm 0.0005$ hours. 1998 SF36 is elongated, with rough global dimension ratios  a/b=2.0, b/c=1.3, but the elongation is not due to a bifurcated shape. The surface is not likely to contain major concavities. No significant albedo variegation was detected.

Key words: solar system: minor planets, asteroids -- techniques: photometric -- methods: numerical

Offprint request: M. Kaasalainen, Mikko.Kaasalainen@astro.helsinki.fi

© ESO 2003

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