Pole coordinates and shape of 30 asteroids

Blanco, C.; Riccioli, D.

doi:10.1051/aas:1998277

Cited by 18 publications

(10 citation statements)

References 15 publications

(17 reference statements)

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“…As the pole solutions were charged with huge values of formal errors (20 • ) they concluded that the spin and shape parameters could be different. Blanco & Riccioli (1998) used the same observational data and the AM-method, obtained similar results (Table 3).…”

Section: Europasupporting

confidence: 54%

Photometry and models of selected main belt asteroids I. 52 Europa, 115 Thyra, and 382 Dodona

Michałowski

Kwiatkowski

Kaasalainen

et al. 2004

A&A

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Section: Europasupporting

confidence: 54%

Photometry and models of selected main belt asteroids I. 52 Europa, 115 Thyra, and 382 Dodona

Michałowski

Kwiatkowski

Kaasalainen

et al. 2004

A&A

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“…The latter paper determined the period to be 9.763 h. Stephens (2005) gives a period of 15.98 h based on new data gathered in 2004, but corrects the value to 9.760 h in 2007 (Stephens 2007), thus confirming the period derived by Zappala et al Blanco & Riccioli (1998) made a preliminary pole determination using the amplitude-magnitude method (see Table 3), which was not confirmed by our results.…”

Section: (386) Siegenasupporting

confidence: 56%

Photometry and models of selected main belt asteroids

Marciniak

Bartczak

Santana-Ros

et al. 2012

A&A

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Context. The shapes and spin states of asteroids observed with photometric techniques can be reconstructed using the lightcurve inversion method. The resultant models can then be confirmed or exploited further by other techniques, such as adaptive optics, radar, thermal infrared, stellar occultations, or space probe imaging. Aims. During our ongoing work to increase the set of asteroids with known spin and shape parameters, there appeared a need for displaying the model plane-of-sky orientations for specific epochs to compare models from different techniques. It would also be instructive to be able to track how the complex lightcurves are produced by various asteroid shapes. Methods. Basing our analysis on an extensive photometric observational dataset, we obtained eight asteroid models with the convex lightcurve inversion method. To enable comparison of the photometric models with those from other observing/modelling techniques, we created an on-line service where we allow the inversion models to be orientated interactively. Results. Our sample of objects is quite representative, containing both relatively fast and slow rotators with highly and lowly inclined spin axes. With this work, we increase the sample of asteroid spin and shape models based on disk-integrated photometry to over 200. Three of the shape models obtained here are confirmed by the stellar occultation data; this also allowed independent determinations of their sizes to be made. Conclusions. The ISAM service can be widely exploited for past and future asteroid observations with various, complementary techniques and for asteroid dimension determination.

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“…Observations of 165 Loreley with Keck AO system at 2.1 μm with a pixel scale of 9.94 mas (left). The apparent shape and orientation using the pole solution of Blanco and Riccioli (1998) and ellipse shape is displayed. The measured size ratio (a/b = 1.26 ± 0.08) is in agreement with the one provided by the physical ephemeris (a/b = 1.37).…”

Section: Resultsmentioning

confidence: 99%

“…Using multiple lightcurve observations of the asteroid, Blanco and Riccioli (1998) determined the orientation of its rotational axis and its shape using the amplitude-magnitude method suggested by Zappala (1981). They reported a pole orientation of λ = 159 ± 18 and β = -65 ± 18 in ECB1950 and ellipse ratios a/b = 1.19 and b/c = 1.27.…”

Section: Other Asteroidsmentioning

confidence: 99%

Shape, size and multiplicity of main-belt asteroidsI. Keck Adaptive Optics survey

Marchis

Kaasalainen

Hom

et al. 2006

Icarus

107

101

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This paper presents results from a high spatial resolution survey of 33 main-belt asteroids with diameters >40 km using the Keck II Adaptive Optics (AO) facility. Five of these (45 Eugenia, 87 Sylvia, 107 Camilla, 121 Hermione, 130 Elektra) were confirmed to have satellite. Assuming the same albedo as the primary, these moonlets are relatively small (∼5% of the primary size) suggesting that they are fragments captured after a disruptive collision of a parent body or captured ejecta due to an impact. For each asteroid, we have estimated the minimum size of a moonlet that can positively detected within the Hill sphere of the system by estimating and modeling a 2-σ detection profile: in average on the data set, a moonlet located at 2/100 × R Hill (1/4 × R Hill ) with a diameter larger than 6 km (4 km) would have been unambiguously seen. The apparent size and shape of each asteroid was estimated after deconvolution using a new algorithm called AIDA. The mean diameter for the majority of asteroids is in good agreement with IRAS radiometric measurements, though for asteroids with a D < 200 km, it is underestimated on average by 6-8%. Most asteroids had a size ratio that was very close to those determined by lightcurve measurements. One observation of 104 Klymene suggests it has a bifurcated shape. The bi-lobed shape of 121 Hermione described in Marchis et al. [Marchis, F., Hestroffer, D., Descamps, P., Berthier, J., Laver, C., de Pater, I., 2005c. Icarus 178, 450-464] was confirmed after deconvolution. The ratio of contact binaries in our survey, which is limited to asteroids larger than 40 km, is surprisingly high (∼6%), suggesting that a non-single configuration is common in the main-belt. Several asteroids have been analyzed with lightcurve inversions. We compared lightcurve inversion models for plane-of-sky predictions with the observed images (9 Metis, 52 Europa, 87 Sylvia, 130 Elektra, 192 Nausikaa, and 423 Diotima, 511 Davida). The AO images allowed us to determine a unique photometric mirror pole solution, which is normally ambiguous for asteroids moving close to the plane of the ecliptic (e.g., 192 Nausikaa and 52 Europa). The photometric inversion models agree well with the AO images, thus confirming the validity of both the lightcurve inversion method and the AO image reduction technique.

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Pole coordinates and shape of 30 asteroids

Cited by 18 publications

References 15 publications

Photometry and models of selected main belt asteroids I. 52 Europa, 115 Thyra, and 382 Dodona

Photometry and models of selected main belt asteroids I. 52 Europa, 115 Thyra, and 382 Dodona

Photometry and models of selected main belt asteroids

Shape, size and multiplicity of main-belt asteroidsI. Keck Adaptive Optics survey

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