Issue |
A&A
Volume 650, June 2021
|
|
---|---|---|
Article Number | A129 | |
Number of page(s) | 15 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/202140342 | |
Published online | 17 June 2021 |
Evidence for differentiation of the most primitive small bodies★,★★
1
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS,
Laboratoire Lagrange,
France
e-mail: benoit.carry@oca.eu
2
Aix Marseille Univ, CNRS, LAM, Laboratoire d’Astrophysique de Marseille,
Marseille,
France
3
IMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ Paris 06, Univ. Lille,
France
4
University of Maryland College Park,
College Park,
MD 20742,
USA
5
NASA Goddard Space Flight Center,
Greenbelt,
MD 20771,
USA
6
Institute of Astronomy, Faculty of Mathematics and Physics, Charles University,
V Holešovičkách 2,
18000
Prague,
Czech Republic
7
Space sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège,
Allée du 6 Août 17,
4000
Liège,
Belgium
8
Department of Earth, Atmospheric and Planetary Sciences, MIT,
77 Massachusetts Avenue,
Cambridge,
MA 02139,
USA
9
Mathematics and Statistics, Tampere University,
33014
Tampere,
Finland
10
Astronomical Observatory Institute, Faculty of Physics, Adam Mickiewicz University,
ul. Słoneczna 36,
60-286
Poznań,
Poland
11
Geneva Observatory,
1290
Sauverny,
Switzerland
12
Oukaimeden Observatory, High Energy Physics and Astrophysics Laboratory, Cadi Ayyad University,
Marrakech,
Morocco
13
Astronomical Institute of the Romanian Academy,
5 Cutitul de Argint,
040557
Bucharest,
Romania
14
Jet Propulsion Laboratory, California Institute of Technology,
4800 Oak Grove Drive,
Pasadena,
CA 91109,
USA
15
European Space Agency, ESTEC - Scientific Support Office,
Keplerlaan 1,
Noordwijk
2200 AG,
The Netherlands
16
Institut Polytechnique des Sciences Avancées IPSA,
63 bis Boulevard de Brandebourg,
94200
Ivry-sur-Seine,
France
17
Thirty-Meter-Telescope,
100 West Walnut St, Suite 300,
Pasadena,
CA 91124,
USA
18
Open University, School of Physical Sciences, The Open University,
MK7 6AA,
UK
19
Laboratoire Atmosphères, Milieux et Observations Spatiales, CNRS & Université de Versailles Saint-Quentin-en-Yvelines,
Guyancourt,
France
20
SETI Institute, Carl Sagan Center,
189 Bernado Avenue,
Mountain View,
CA 94043,
USA
21
Sección Física, Departamento de Ciencias, Pontificia Universidad Católica del Perú,
Apartado 1761,
Lima,
Peru
22
Institute of Physics, University of Szczecin,
Wielkopolska 15,
70-453
Szczecin,
Poland
23
Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante, Alicante,
Spain
24
Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB),
Martí Franquès 1,
E08028
Barcelona,
Spain
25
Towson University,
Towson,
MD,
USA
26
Center for Solar System Studies,
446 Sycamore Ave.,
Eaton,
CO 80615,
USA
27
European Southern Observatory (ESO),
Alonso de Cordova 3107,
1900
Casilla Vitacura,
Santiago,
Chile
Received:
14
January
2021
Accepted:
5
March
2021
Context. Dynamical models of Solar System evolution have suggested that the so-called P- and D-type volatile-rich asteroids formed in the outer Solar System beyond Neptune’s orbit and may be genetically related to the Jupiter Trojans, comets, and small Kuiper belt objects (KBOs). Indeed, the spectral properties of P- and D-type asteroids resemble that of anhydrous cometary dust.
Aims. We aim to gain insights into the above classes of bodies by characterizing the internal structure of a large P- and D-type asteroid.
Methods. We report high-angular-resolution imaging observations of the P-type asteroid (87) Sylvia with the Very Large Telescope Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) instrument. These images were used to reconstruct the 3D shape of Sylvia. Our images together with those obtained in the past with large ground-based telescopes were used to study the dynamics of its two satellites. We also modeled Sylvia’s thermal evolution.
Results. The shape of Sylvia appears flattened and elongated (a/b ~1.45; a/c ~1.84). We derive a volume-equivalent diameter of 271 ± 5 km and a low density of 1378 ± 45 kg m−3. The two satellites orbit Sylvia on circular, equatorial orbits. The oblateness of Sylvia should imply a detectable nodal precession which contrasts with the fully-Keplerian dynamics of its two satellites. This reveals an inhomogeneous internal structure, suggesting that Sylvia is differentiated.
Conclusions. Sylvia’s low density and differentiated interior can be explained by partial melting and mass redistribution through water percolation. The outer shell should be composed of material similar to interplanetary dust particles (IDPs) and the core should be similar to aqueously altered IDPs or carbonaceous chondrite meteorites such as the Tagish Lake meteorite. Numerical simulations of the thermal evolution of Sylvia show that for a body of such a size, partial melting was unavoidable due to the decay of long-lived radionuclides. In addition, we show that bodies as small as 130–150 km in diameter should have followed a similar thermal evolution, while smaller objects, such as comets and the KBO Arrokoth, must have remained pristine, which is in agreement with in situ observations of these bodies. NASA Lucy mission target (617) Patroclus (diameter ≈140 km) may, however, be differentiated.
Key words: minor planets, asteroids: general / Kuiper belt: general / minor planets, asteroids: individual: Sylvia
Tables A.1, B.1, C.1 and C.2 and the reduced and deconvolved SPHERE images are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/650/A129
Based on observations made with ESO telescopes at the La Silla Paranal Observatory under program 073.C-0851 (PI Merline), 073.C-0062 (PI Marchis), 085.C-0480 (PI Nitschelm), 088.C-0528 (PI Rojo), 199.C-0074 (PI Vernazza).
© B. Carry et al. 2021
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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