Full Adaptive Optics Images of Asteroids Ceres and Vesta; Rotational Poles and Triaxial Ellipsoid Dimensions

Drummond, Jack D.; Fugate, Robert Q.; Christou, Julian C.; Hege, E. K.

doi:10.1006/icar.1997.5882

Cited by 64 publications

(47 citation statements)

References 26 publications

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“…1. The Rosetta P syn is slightly longer, but still compatible within the error bars, than the very precise value of the sidereal period (5.34212971 ± 0.00000096 h) derived by Drummond et al (1998).…”

Section: Lightcurve and Phase Functionsupporting

confidence: 60%

Photometric observations of asteroid 4 Vesta by the OSIRIS cameras onboard the Rosetta spacecraft

Fornasier

Mottola²,

Barucci

et al. 2011

A&A

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Aims. We report on new observations of asteroid 4 Vesta obtained on 1 May 2010 with the optical system OSIRIS onboard the ESA Rosetta mission. One lightcurve was taken at a phase angle (52 • ) larger than achievable from ground-based observations together with a spectrophotometric sequence covering the 260 to 990 nm wavelength range. Methods. Aperture photometry was used to derive the Vesta flux at several wavelengths. A Fourier analysis and the HG system formalism were applied to derive the Vesta rotational period and characterize its phase function. Results. We find a G parameter value of 0.27 ± 0.01 and an absolute magnitude H(R) = 2.80 ± 0.01. The lightcurve has the largest amplitude ever reported for Vesta (0.19 ± 0.01 mag), and we derive a synodic rotational period of 5.355 ± 0.025 h. The Rosetta spectrophotometry, covering the Vesta western hemisphere, is in perfect agreement with visible spectra from the literature and close to the IUE observations related to the same hemisphere. The new spectrophotometric data reveal that there is no global ultraviolet/visible reversal on Vesta. The Vesta spectrophotometry is well reproduced by spectra of howardite meteorite powders (grain size <25 μm). From the Rosetta absolute spectrophotometry and from the phase function behaviour, we estimate a geometric albedo of 0.36 ± 0.02 at 649 nm and 0.34 ± 0.02 at 535 nm.

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Section: Lightcurve and Phase Functionsupporting

confidence: 60%

Photometric observations of asteroid 4 Vesta by the OSIRIS cameras onboard the Rosetta spacecraft

Fornasier

Mottola²,

Barucci

et al. 2011

A&A

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“…With the knowledge that Lundia is a V-type object, we can assume Vesta-like albedo. However, a Vesta albedo may differ by about 20% between the darkest and brightest areas of the surface of Vesta as suggested by Binzel et al (1997) using HST data, and Drummond et al (1998) using a ground-based adaptive optics system. Therefore, depending on which part of Vesta was observed, the albedo might differ significantly from the IRAS result of p V = 0.42.…”

Section: Modellingmentioning

confidence: 96%

New binary asteroid 809 Lundia

Kryszczyńska¹,

Colas

Descamps

et al. 2009

A&A

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• , β = 28 ± 4• (modified Roche) or λ = 120 ± 5 • , β = 18 ± 12 • (kinematic). Triaxial ellipsoid shape solutions and a separation between components of 15.8 km are given after taking an equivalent diameter of 9.1 km from H = 11.8 mag and assuming an albedo of 0.4. The orbital period of the Lundia system obtained from modelling is the same as from the lightcurve analysis i.e., 15.418 ± 0.001 h. The bulk density of both components is 1.64 or 1.71 ± 0.01 g/cm 3 . The double system of Lundia probably originates from the fission process of a single body that could have been spun up by the YORP effect. The predicted lightcurves for future oppositions are also presented.

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“…Several near-Earth asteroids have been imaged by radar (Hudson et al 2003;Benner et al 2002), and several main belt asteroids have been imaged with speckle interferometry (McCarthy et al 1994;Ragazzoni et al 2000) and AO (Saint-Pe et al 1993;Drummond et al 1998;Hestroffer et al 2002;Baliunas et al 2003). For the most part near-Earth asteroids are too faint for speckle interferometry and AO systems.…”

Section: Imagesmentioning

confidence: 99%

Characterization of the near-Earth Asteroid 2002 NY40

Roberts¹,

Hall²,

Lambert³

et al. 2007

Icarus

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In August 2002, the near-Earth asteroid 2002 NY 40 , made its closest approach to the Earth. This provided an opportunity to study a near-Earth asteroid with a variety of instruments. Several of the telescopes at the Maui Space Surveillance System were trained at the asteroid and collected adaptive optics images, photometry and spectroscopy. Analysis of the imagery reveals the asteroid is triangular shaped with significant self-shadowing.The photometry reveals a 20-hour period and the spectroscopy shows that the asteroid is a Q-type.

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Full Adaptive Optics Images of Asteroids Ceres and Vesta; Rotational Poles and Triaxial Ellipsoid Dimensions

Cited by 64 publications

References 26 publications

Photometric observations of asteroid 4 Vesta by the OSIRIS cameras onboard the Rosetta spacecraft

Photometric observations of asteroid 4 Vesta by the OSIRIS cameras onboard the Rosetta spacecraft

New binary asteroid 809 Lundia

Characterization of the near-Earth Asteroid 2002 NY40

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