Lightcurve and Radar Observations and Analysis of 11 Parthenope and 678 Fredegundis

Details Lightcurve and Radar Observations and Analysis of 11 Parthenope and 678 Fredegundis Lightcurve and Radar Observations and Analysis of 11 Parthenope and 678 Fredegundis

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.2816s&link_type=abstract

American Astronomical Society, DPS meeting #40, #28.16; Bulletin of the American Astronomical Society, Vol. 40, p.439

Astronomy and Astrophysics

Astronomy

Scientific paper

We present results from extended campaigns in 2008 on main-belt asteroids 11 Parthenope and 678 Fredegundis.
11 Parthenope has been observed for several apparitions but the rotation period remained uncertain, with values between 5 and 13.7 h being reported (http:/www.MinorPlanetObserver.com/astlc/default.htm). Part of the uncertainty can be attributed to the low amplitude of the lightcurve, 0.05 to 0.12 mag, which can lead to ambiguous period solutions. Using internally calibrated data, we determined an unambiguous synodic period of 13.734 ± 0.001 h, which agrees with that reported by Lang and Hansen (1999, Minor Planet Bul. 26, 15-18). We expect to obtain a very precise phase relation with accurate H, G parameters, but minimum phase angle does not occur until after the abstract deadline.
678 Fredegundis was observed in support of radar observations by Shepard. The radar observations indicate the possibility of a bifurcated or "contact binary" object. The lightcurve showed considerable evolution of features during the campaign that covered phase angles from 1 to 22 degrees. The synodic period was firmly established at 11.61624 ± 0.00014 h. We also determined the absolute magnitude, HR = 8.793 ± 0.007, slope parameter G = 0.20 ± 0.01, and color index, V-R = 0.40 ± 0.05. The lightcurve is suggestive of a "contact binary", but can also be fit by a brick shaped convex hull. This illustrates the difficulty of inferring concavities from lightcurve inversion.
Funding for Shepard was provided by NSF grant AST 0605903. Funding for Warner and Harris was provided by NASA grant NNG06GI32G and by NSF grant AST-0607505.

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