B. D. Warner, Palmer Divide Observatory and Space Science Institute, Colorado Springs, CO, U.S.A.; P. Pravec, Ondrejov Observatory; A. W. Harris, Space Science Institute, La Canada, CA, U.S.A.; D. Higgins, Hunters Hill Observatory, Ngunnawal, ACT, Australia; C. Bembrick, Mt. Tarana Observatory, Bathurst, NSW, Australia; and J. Brinsfield, Via Capote Observatory, Thousand Oaks, CA, U.S.A. report that photometric observations obtained during Feb. 28-Mar. 8 reveal that minor planet (2577) is a binary system with an orbital period of 35.78 +/- 0.05 hr. The primary shows a period of 2.8141 +/- 0.0006 hr, and it has a lightcurve amplitude of 0.24 mag. Mutual eclipse/occultation events indicate a secondary-to-primary mean-diameter ratio of 0.35 +/- 0.02. The periods and amplitudes were determined using a subset of data (Mar. 4-8). Data on Feb. 28 and Mar. 1 show no events and fit the same primary period, but the lightcurve has a slightly different shape; this may indicate that the primary lightcurve is evolving with changing viewing aspect, and so additional observations are warranted as the moon clears the area.
Central Bureau Electronic Telegrams
- Pub Date:
- March 2009