Three-dimensional reconstruction using multiresolution photoclinometry by deformation

Capanna, Claire; Gesquière, Gilles; Jordá, L.; Lamy, P.; Vibert, D.

doi:10.1007/s00371-013-0821-5

Cited by 20 publications

(15 citation statements)

References 12 publications

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“…A.4. We then applied the so-called Multi-resolution PhotoClinometry by Deformation (MPCD) method (Capanna et al 2013;Jorda et al 2016) on our sample of 35 VLT/SPHERE/ZIMPOL images from 12 different epochs to reconstruct the 3D shape of Psyche. This method gradually deforms the vertices of an initial mesh to minimize the difference between the observed images and synthetic images of the deformed model created with the OASIS software (Optimized Astrophysical Simulator for Imaging Systems; Jorda et al 2010).…”

Section: Methods: Three-dimensional Shape Reconstructionmentioning

confidence: 99%

Asteroid (16) Psyche’s primordial shape: A possible Jacobi ellipsoid

Ferrais

Vernazza

Jordá

et al. 2020

A&A

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Context. Asteroid (16) Psyche is the largest M-type asteroid in the main belt and the target of the NASA Psyche mission. It is also the only asteroid of this size (D > 200 km) known to be metal rich. Although various hypotheses have been proposed to explain the rather unique physical properties of this asteroid, a perfect understanding of its formation and bulk composition is still missing. Aims. We aim to refine the shape and bulk density of (16) Psyche and to perform a thorough analysis of its shape to better constrain possible formation scenarios and the structure of its interior. Methods. We obtained disk-resolved VLT/SPHERE/ZIMPOL images acquired within our ESO large program (ID 199.C-0074), which complement similar data obtained in 2018. Both data sets offer a complete coverage of Psyche’s surface. These images were used to reconstruct the three-dimensional (3D) shape of Psyche with two independent shape modeling algorithms (MPCD and ADAM). A shape analysis was subsequently performed, including a comparison with equilibrium figures and the identification of mass deficit regions. Results. Our 3D shape along with existing mass estimates imply a density of 4.20 ± 0.60 g cm−3, which is so far the highest for a solar system object following the four telluric planets. Furthermore, the shape of Psyche presents small deviations from an ellipsoid, that is, prominently three large depressions along its equator. The flatness and density of Psyche are compatible with a formation at hydrostatic equilibrium as a Jacobi ellipsoid with a shorter rotation period of ∼3h. Later impacts may have slowed down Psyche’s rotation, which is currently ∼4.2 h, while also creating the imaged depressions. Conclusions. Our results open the possibility that Psyche acquired its primordial shape either after a giant impact while its interior was already frozen or while its interior was still molten owing to the decay of the short-lived radionuclide 26Al.

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Section: Methods: Three-dimensional Shape Reconstructionmentioning

confidence: 99%

Asteroid (16) Psyche’s primordial shape: A possible Jacobi ellipsoid

Ferrais

Vernazza

Jordá

et al. 2020

A&A

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“…We used a new method called "Multi-resolution PhotoClinometry by Deformation" (hereafter MPCD) developed by Capanna et al (2013) to reconstruct the global shape of the comet from images acquired during the "SHAP1" rotational movie (see section 3.1 and Table 2). The method applies deformation to the vertices of a triangular mesh, initially a sphere of radius 1.9 km , until synthetic images of the deformed shape model match the observed ones ( Fig.…”

Section: Early Reconstruction With Mpcdmentioning

confidence: 99%

The global shape, density and rotation of Comet 67P/Churyumov-Gerasimenko from preperihelion Rosetta/OSIRIS observations

Jordá

Gaskell

Capanna

et al. 2016

Icarus

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“…With a mean diameter of about 100 km, Lutetia is more than two times larger than the previously imaged asteroids (Table 1). The global shape of Lutetia was reconstructed from the images (Gaskell et al, 2008;Jorda et al, 2011;Preusker et al, 2012;Capanna et al, 2013) and different surface features such as lineaments, landslides, boulders and impact craters were identified (Küppers et al, 2012;Thomas et al, 2012). Impact cratering is a fundamental process in the Solar System and the main process by which asteroid surfaces are shaped.…”

Section: Introductionmentioning

confidence: 99%