Asteroid Photometric and Polarimetric Phase Effects

Muinonen, K.; Piironen, J.; Shkuratov, Yu. G.; Ovcharenko, Andrey; Clark, B. E.

doi:10.2307/j.ctv1v7zdn4.16

Cited by 96 publications

(42 citation statements)

References 91 publications

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“…24) Themis) and L-type (e.g. ( 12) Victoria) asteroids, respectively (Muinonen et al 2002;Gil-Hutton et al 2008). Fig.…”

Section: Discussionmentioning

confidence: 99%

“…The circular polarization values in all cases are consistent with a zero signal to within 2.5σ, and thus we do not detect any circular polarization of the light scattered from these asteroids. Circular polarization is predicted to appear on asteroids that have surfaces containing powdered metals, especially those with highly irregular shapes (Degtjarev & Kolokolova 1992), however circular polarization as of yet has not been detected from an asteroid (e.g., Muinonen et al 2002).…”

Section: Observationsmentioning

confidence: 99%

“…In addition, two comparison phase curves are also plotted. The first is the fit by Muinonen et al (2002) to polarization data from (24) Themis, a member of the B taxonomic class. B-type and C-type asteroids typically show the deepest negative polarization branches.…”

Section: Observationsmentioning

confidence: 99%

“…The polarimetric effect in this theory has a strong dependence on the size and spacing of the scattering particles meaning that surface chemistry and mineralogy should play a large role in determining the polarization as a function of phase. According to Muinonen et al (2002), coherent backscattering is the key physical process generating both these effects.…”

Section: Introductionmentioning

confidence: 99%

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Polarization of Asteroid (387) Aquitania: The newest member of a class of large inversion angle asteroids

Masiero¹,

Cellino²

2009

Icarus

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We present new imaging polarimetric observations of two Main Belt asteroids, (234) Barbara and (387) Aquitania, taken in the first half of 2008 using the Dual-Beam Imaging Polarimeter on the University of Hawaii 2.2 meter telescope, located on Mauna Kea, Hawaii. Barbara had been previously shown to exhibit a very unusual polarization-phase curve by Cellino et al. (2006). Our observations confirm this result and add Aquitania to the growing class of large inversion angle objects. Interestingly, these asteroids show spinel features in their IR spectra suggesting a mineralogical origin to the phase angle-dependent polarimetric features. As spinel is associated with calcium-aluminum-rich inclusions and carbonaceous chondrites, these large inversion angle asteroids may represent some of the oldest surfaces in the solar system. Circular as well as linear polarization measurements were obtained but circular polarization was not detected.

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“…24) Themis) and L-type (e.g. ( 12) Victoria) asteroids, respectively (Muinonen et al 2002;Gil-Hutton et al 2008). Fig.…”

Section: Discussionmentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Polarization of Asteroid (387) Aquitania: The newest member of a class of large inversion angle asteroids

Masiero¹,

Cellino²

2009

Icarus

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“…For an assumed linear phase function the notation φ(α) = 10 −0.4βα , where β is the "linear" phase coefficient, is used. Using data from Table 1 along with an S-type asteroid albedo of 0.1 and a linear phase coefficient of β = 0.03 mags per degree, as found for Mercury and S-type asteroids (Veverka et al 1988;Muinonen et al 2002), shows that 20.4 magnitudes corresponds to satellites that are about 0.3 km (300 meters) in radius at Venus' observing geometry. Figures 2 and 3 show how the satellite radius corresponds to the survey's detection efficiency.…”

Section: Analysis and Resultsmentioning

confidence: 78%

A survey for satellites of Venus

Sheppard

Trujillo

2009

Icarus

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We present a systematic survey for satellites of Venus using the BaadeMagellan 6.5 meter telescope and IMACS wide-field CCD imager at Las Campanas observatory in Chile. In the outer portions of the Hill sphere the search was sensitive to a limiting red magnitude of about 20.4, which corresponds to satellites with radii of a few hundred meters when assuming an albedo of 0.1. In the very inner portions of the Hill sphere scattered light from Venus limited the detection to satellites of about a kilometer or larger. Although several main belt asteroids were found, no satellites (moons) of Venus were detected.

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