Photometric geodesy of main-belt asteroids

Weidenschilling, S. J.; Chapman, C. R.; Davis, Donald R.; Greenberg, R.; Levy, David H.; Binzel, Richard P.; Vail, S.; Magee, M.; Spaute, D.

doi:10.1016/0019-1035(90)90227-z

Cited by 47 publications

(33 citation statements)

References 24 publications

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“…The first photometric observations for this asteroid were reported by Weidenschilling et al (1990). They observed 7.356 ± 0.001 hours and an amplitude of 0.22 mag was determined.…”

Section: Henriettamentioning

confidence: 93%

CCD photometry, spin and shape models of five asteroids: 225, 360, 416, 516, and 1223

Michałowski

Pych

Berthier

et al. 2000

Astron. Astrophys. Suppl. Ser.

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Abstract. New CCD photometric observations for 225 Henrietta (1995), 360 Carlova (1996, 1997, 1998), 416 Vaticana (1995-96, 1998), 516 Amherstia (1995, 1996, and 1223 Neckar (1995-96) carried out at five observatories are presented. New synodical periods for two asteroids (225, 1223) have been obtained. Using all available lightcurves, the spin vectors, senses of rotation, and triaxial elipsoid models of these five asteroids have been determined or refined.

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“…The first photometric observations for this asteroid were reported by Weidenschilling et al (1990). They observed 7.356 ± 0.001 hours and an amplitude of 0.22 mag was determined.…”

Section: Henriettamentioning

confidence: 93%

CCD photometry, spin and shape models of five asteroids: 225, 360, 416, 516, and 1223

Michałowski

Pych

Berthier

et al. 2000

Astron. Astrophys. Suppl. Ser.

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“…Observed previously by Weidenschilling et al (1990) For the modelling, we were able to use our data from three apparitions coupled with data from 2005 provided by Menke et al (2008), from 2006 by Behrend et al (www), and only one of the four lightcurves from 1986 saved as a composit by Weidenschillig (1990). In total, there are 60 lightcurve fragments from six apparitions.…”

Section: (329) Sveamentioning

confidence: 99%

“…However, some of the observations only partially covered its 13.34-hour lightcurve (Weidenschilling et al 1990;Shevchenko et al 1992;Neely 1992;Schober et al 1994;Ferrero 2014, Behrend et al, www). Erikson et al (2000), and Tungalag et al (2002) published spin and shape solution for Venetia with similar spin axis coordinates, but a notable difference in sidereal period: Erikson et al (2000) …”

Section: (487) Venetiamentioning

confidence: 99%

Photometric survey, modelling, and scaling of long-period and low-amplitude asteroids

Marciniak

Bartczak

Müller

et al. 2018

A&A

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Context. The available set of spin and shape modelled asteroids is strongly biased against slowly rotating targets and those with low lightcurve amplitudes. This is due to the observing selection effects. As a consequence, the current picture of asteroid spin axis distribution, rotation rates, radiometric properties, or aspects related to the object's internal structure might be affected too. Aims. To counteract these selection effects, we are running a photometric campaign of a large sample of main belt asteroids omitted in most previous studies. Using least chi-squared fitting we determined synodic rotation periods and verified previous determinations. When a dataset for a given target was sufficiently large and varied, we performed spin and shape modelling with two different methods to compare their performance. Methods. We used the convex inversion method and the non-convex SAGE algorithm, applied on the same datasets of dense lightcurves. Both methods search for the lowest deviations between observed and modelled lightcurves, though using different approaches. Unlike convex inversion, the SAGE method allows for the existence of valleys and indentations on the shapes based only on lightcurves. Results. We obtain detailed spin and shape models for the first five targets of our sample: (159) Aemilia, (227) Philosophia, (329) Svea, (478) Tergeste, and (487) Venetia. When compared to stellar occultation chords, our models obtained an absolute size scale and major topographic features of the shape models were also confirmed. When applied to thermophysical modelling, they provided a very good fit to the infrared data and allowed their size, albedo, and thermal inertia to be determined. Conclusions. Convex and non-convex shape models provide comparable fits to lightcurves. However, some non-convex models fit notably better to stellar occultation chords and to infrared data in sophisticated thermophysical modelling (TPM). In some cases TPM showed strong preference for one of the spin and shape solutions. Also, we confirmed that slowly rotating asteroids tend to have higher-than-average values of thermal inertia, which might be caused by properties of the surface layers underlying the skin depth.

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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%

DAMIT: a database of asteroid models

Ďurech

Sidorin

Kaasalainen

2010

A&A

243

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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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Photometric geodesy of main-belt asteroids

Cited by 47 publications

References 24 publications

CCD photometry, spin and shape models of five asteroids: 225, 360, 416, 516, and 1223

CCD photometry, spin and shape models of five asteroids: 225, 360, 416, 516, and 1223

Photometric survey, modelling, and scaling of long-period and low-amplitude asteroids

DAMIT: a database of asteroid models

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