Photometry and models of selected main belt asteroids

Marciniak, A.; Michałowski, Tadeusz; Hirsch, R.; Behrend, R.; Bernasconi, L.; Descamps, P.; Colas, François; Sobkowiak, K.; Kamiński, K.; Kryszczyńska, A.; Kwiatkowski, T.; Polińska, M.; Rudawska, Regina; Fauvaud, S.; Santacana, G.; Bruno, Alain; Fauvaud, M.; Teng-Chuen-Yu, J.-P.; Peyrot, A.

doi:10.1051/0004-6361/200912741

Cited by 10 publications

(1 citation statement)

References 20 publications

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“…One way how to test the reliability of models based only on CSS data is to compare them with models derived from different photometric data set. So far, about a hundred of asteroid models were derived from dense data (e.g., Kaasalainen et al, 2002;Torppa et al, 2003;Slivan et al, 2003;Marciniak et al, 2007;Ďurech et al, 2007), another ∼ 100 models were derived from combined dense and sparse data (Ďurech et al, 2009;Hanuš et al, 2011). These models are believed to be reliable and thus correct.…”

Section: Reliability Of Asteroid Models Derived Only From the Catalinmentioning

confidence: 99%

The potential of sparse photometric data in asteroid shape modeling

Hanuš¹,

Ďurech²

2012

Planetary and Space Science

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We investigate the potential of the sparse data produced by the Catalina Sky Survey astrometric project (CSS for short) in asteroid shape and rotational state determination by the lightcurve inversion method. We show that although the photometric quality of the CSS data, compared to the dense data, is significantly worse, it is in principle possible that these data are for some asteroids with high lightcurve amplitudes sufficient for a unique shape determination. CSS data are available for ∼ 180 asteroids for which shape models were previously derived from different photometric data sets. For 13 asteroids from this sample, we derive their unique shape models based only on CSS data, compare the two independent shape models together and discuss the reliability of models derived from only CSS data. We also use CSS data to determine shape models for asteroids with already known rotational period values, derive 12 unique models and compare previously published periods with periods determined from the full 3D modeling by the lightcurve inversion method. Finally, we test different shape resolutions used in the lightcurve inversion method in order to find reliable asteroid models.

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Section: Reliability Of Asteroid Models Derived Only From the Catalinmentioning

confidence: 99%

The potential of sparse photometric data in asteroid shape modeling

Hanuš¹,

Ďurech²

2012

Planetary and Space Science

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Thermophysical modeling of asteroids from WISE thermal infrared data – Significance of the shape model and the pole orientation uncertainties

Hanuš

Delbò

Ďurech

et al. 2015

Icarus

116

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In the analysis of thermal infrared data of asteroids by means of thermophysical models (TPMs) it is a common practice to neglect the uncertainty of the shape model and the rotational state, which are taken as an input for the model.Here, we present a novel method of investigating the importance of the shape model and the pole orientation uncertainties in the thermophysical modeling -the varied shape TPM (VS-TPM). Our method uses optical photometric data to generate various shape models that map the uncertainty in the shape and the rotational state. The TPM procedure is then run for all these shape models. We apply the implementation of the classical TPM as well as our VS-TPM to the convex shape models of several asteroids together with their thermal infrared data acquired by the NASA's Wide-field Infrared Survey Explorer (WISE) and compare the results. These show that the uncertainties of the shape model and the pole orientation can be very important (e.g., for the determination of the thermal inertia) and should be considered in the thermophysical analyses. We present thermophysical properties for six asteroids -(624) Hektor, (771) Libera, (1036) Ganymed, (1472) Muonio, (1627) Ivar, and (2606) Odessa.

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Spin states of asteroids in the Eos collisional family

Hanuš

Delbò

Alí-Lagoa

et al. 2018

Icarus

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Eos family was created during a catastrophic impact about 1.3 Gyr ago. Rotation states of individual family members contain information about the history of the whole population. We aim to increase the number of asteroid shape models and rotation states within the Eos collision family, as well as to revise previously published shape models from the literature. Such results can be used to constrain theoretical collisional and evolution models of the family, or to estimate other physical parameters by a thermophysical modeling of the thermal infrared data. We use all available disk-integrated optical data (i.e., classical dense-in-time photometry obtained from public databases and through a large collaboration network as well as sparse-in-time individual measurements from a few sky surveys) as input for the convex inversion method, and derive 3D shape models of asteroids together with their rotation periods and orientations of rotation axes. We present updated shape models for 15 asteroids and new shape model determinations for 16 asteroids. Together with the already published models from the publicly available DAMIT database, we compiled a sample of 56 Eos family members with known shape models that we used in our analysis of physical properties within the family. Rotation states of asteroids smaller than ~20 km are heavily influenced by the YORP effect, whilst the large objects more or less retained their rotation state properties since the family creation. Moreover, we also present a shape model and bulk density of asteroid (423) Diotima, an interloper in the Eos family, based on the disk-resolved data obtained by the Near InfraRed Camera (Nirc2) mounted on the W.M. Keck II telescope.Comment: Accepted for publication in ICARUS Special Issue - Asteroids: Origin, Evolution & Characterizatio

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Photometry and models of selected main belt asteroids

Cited by 10 publications

References 20 publications

The potential of sparse photometric data in asteroid shape modeling

The potential of sparse photometric data in asteroid shape modeling

Thermophysical modeling of asteroids from WISE thermal infrared data – Significance of the shape model and the pole orientation uncertainties

Spin states of asteroids in the Eos collisional family

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