Asteroid lightcurve observations from 1981

Harris, Alan W.; Young, James W.; Dockweiler, Thor; Gibson, J. E.; Poutanen, Markku; Bowell, E.

doi:10.1016/0019-1035(92)90195-d

Cited by 63 publications

(55 citation statements)

References 19 publications

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“…Our Keck AO observed with a/b = 1.34 ± 0.15 is in better agreement with the Δm = 0.16 (a/ b = 1.16) by Harris et al (1992) than Δm = 0.08 reported by Shevchenko et al (1992), implying that the geometry of observations during Harris' and our observations was similar. The Keck AO mean size of 79 km is very close to the D IRAS = 83 km.…”

Section: Other Asteroidssupporting

confidence: 88%

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

Marchis

Kaasalainen

Hom

et al. 2006

Icarus

109

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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Section: Other Asteroidssupporting

confidence: 88%

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

Marchis

Kaasalainen

Hom

et al. 2006

Icarus

109

101

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“…USNO stands for the US Naval Observatory in Flagstaff -the photometry obtained at this observatory as a by-product of astrometric observations was downloaded from the AstDys page 4 and used for modelling. Scaltriti & Zappala (1977c) Zappala et al (1983a (54) Alexandra Belskaya et al (1993) di Martino et al (1987b) Haupt & Hanslmeier (1985 Tancredi & Gallardo (1991) USNO van Houten- (55) Pandora Barucci et al (1985) di Martino & Cacciatori (1984a) di Martino et al (1987b) Lagerkvist et al (1995) Shevchenko et al (1993 Schober ( Zappala et al (1982) (129) Antigone Barucci et al (1985) di Martino & Cacciatori (1984a) di Martino et al (1987b) Dotto et al (1992 Scaltriti & Zappala (1977b) Torppa et al (2003) Vesely & Taylor (1985) Weidenschilling et al (1987) Weidenschilling et al (1990 (130) Elektra Danforth & Ratcliff (1994) Debehogne et al (1990) Durech et al (2007) Harris & Young (1989 Harris et al (1999) Shevchenko et al (1996) Weidenschilling et al (1987 (132) Aethra USNO Weidenschilling et al (1990) Wisniewski et al (1997 (135) Hertha Dotto et al (1992) Harris et al (1992) Lagerkvist ( Zappala et al (1983b) (770) Bali USNO W...…”

Section: Appendix A: Lightcurve Referencesmentioning

confidence: 99%

“…Hainaut- Rouelle et al (1995) Harris et al (1992) Schober (1979) (849) Ara Harris et al (1992) Marciniak et al (2009b) Pravec et al (1997) …”

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confidence: 99%

DAMIT: a database of asteroid models

Ďurech

Sidorin

Kaasalainen

2010

A&A

249

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Context. Apart from a few targets that were directly imaged by spacecraft, remote sensing techniques are the main source of information about the basic physical properties of asteroids, such as the size, the spin state, or the spectral type. The most widely used observing technique -time-resolved photometry -provides us with data that can be used for deriving asteroid shapes and spin states. In the past decade, inversion of asteroid lightcurves has led to more than a hundred asteroid models. In the next decade, when data from all-sky surveys are available, the number of asteroid models will increase. Combining photometry with, e.g., adaptive optics data produces more detailed models. Aims. We created the Database of Asteroid Models from Inversion Techniques (DAMIT) with the aim of providing the astronomical community access to reliable and up-to-date physical models of asteroids -i.e., their shapes, rotation periods, and spin axis directions. Models from DAMIT can be used for further detailed studies of individual objects, as well as for statistical studies of the whole set. Methods. Most DAMIT models were derived from photometric data by the lightcurve inversion method. Some of them have been further refined or scaled using adaptive optics images, infrared observations, or occultation data. A substantial number of the models were derived also using sparse photometric data from astrometric databases.Results. At present, the database contains models of more than one hundred asteroids. For each asteroid, DAMIT provides the polyhedral shape model, the sidereal rotation period, the spin axis direction, and the photometric data used for the inversion. The database is updated when new models are available or when already published models are updated or refined. We have also released the C source code for the lightcurve inversion and for the direct problem (updates and extensions will follow).

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“…The first photometric observations of (76) Freia were performed by Harris & Young (1983) in 1979, yielding a synodic period value of 9.79 h. Further observations were obtained in 1981 by Lagerkvist et al (1987) and Harris et al (1992). The latter work reported a synodic period of 9.972 h. In 1984, (76) Freia was obseved again, with a determined period of 9.98 h (Lagerkvist et al 1986).…”

Section: (76) Freiamentioning

confidence: 96%

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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Asteroid lightcurve observations from 1981

Cited by 63 publications

References 19 publications

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

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

DAMIT: a database of asteroid models

Photometry and models of selected main belt asteroids

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