1998
DOI: 10.1006/icar.1998.5991
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Photometric Properties of Asteroid 4179 Toutatis from Lightcurves and a Radar-Derived Physical Model

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Cited by 29 publications
(28 citation statements)
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“…Significant new parts of rotational cycles cannot be obtained during one night, so the absolute magnitude should be calibrated very accurately. As the lightcurve fit of Hudson & Ostro (1998) (based on radar observations) shows, this is not the case, and we should expect the corresponding noise to be of order 0.1 mag. Lightcurve analysis without prior information confirms this.…”
Section: An Obvious Example Of Real Observations Is 4179mentioning
confidence: 99%
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“…Significant new parts of rotational cycles cannot be obtained during one night, so the absolute magnitude should be calibrated very accurately. As the lightcurve fit of Hudson & Ostro (1998) (based on radar observations) shows, this is not the case, and we should expect the corresponding noise to be of order 0.1 mag. Lightcurve analysis without prior information confirms this.…”
Section: An Obvious Example Of Real Observations Is 4179mentioning
confidence: 99%
“…I simply adopted the values P ψ = 7.35, P φ = 5.41 days as the data do not lend themselves to an accurate analysis; many nearby values would have given equally good fits. Only the observations at solar phase angles less than 90 • were included to minimize the uncertainties due to Hudson & Ostro (1998). The respective initial Euler angles of the two types of fit are within a few degrees from each other, except for ψ 0 that varies some twenty degrees as its role is not very significant, the inertia ellipsoid being almost axisymmetric.…”
Section: An Obvious Example Of Real Observations Is 4179mentioning
confidence: 99%
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“…It has closely encountered the Earth every four years during the last decade, enabling a variety of ground-based assessments. Radar observations generated by Arecibo and Goldstone reveal the irregular shape with two lobes and the tumbling, non-principal axis (NPA) rotating state of the asteroid Hudson et al 1998;Ostro et al 1999Ostro et al , 2002Hudson et al 2003). Spencer et al (1995) calculated two rotational periods of the complicated spin state, which were 7.3 and 3.1 days using optical data acquired during 1992 flyby.…”
Section: Introductionmentioning
confidence: 99%