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Communication Dans Un Congrès Année : 2022

Search for rings around the large Trans-Neptunian Object (50000) Quaoar 

Bruno Sicardy
Bruno Morgado
Felipe Braga-Ribas
Jose Luis Ortiz
Chrystian Pereira
Roberto Viera-Martins
  • Fonction : Auteur
Heikki Salo
Thamiris de Santana
  • Fonction : Auteur
Rafael Sfair
  • Fonction : Auteur
Marcelo Assafin
  • Fonction : Auteur
Gustavo Benedetti-Rossi
Julio Camargo
  • Fonction : Auteur
Estela Fernandez-Valenzuela
Altair Gomes-Júnior
Mike Kretlow
Flavia Rommel
Pablo Santos-Sanz
Damya Souami
  • Fonction : Auteur
Frédéric Vachier
  • Fonction : Auteur

Résumé

<p>The Trans-Neptunian Object (50000) Quaoar, classified as a cubewano, is a dwarf planet candidate with a diameter of 1110 km [Br13], semi-major axis of 43.7 au and orbital eccentricity of 0.04. Its satellite Weywot orbits at 13,300 km from the primary object, and from its flux [Fr10], its diameter is about 90 km, assuming the same albedo as Quaoar. Several campaigns were conducted under the umbrella of the Lucky Star project (https://lesia.obspm.fr/lucky-star/) to observe stellar occultations by Quaoar and Weywot. Besides measuring Quaoar's and Weywot's size and shapes, those campaigns aimed at searching for material around Quaoar.</p><p>Here, we will present the results of our search for rings around Quaoar based on the following observations:&#160;</p><p>Dates &#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160; Places of observations<br>2 September 2018&#160;&#160; Namibia<br>5 June 2019 &#160; &#160; &#160; &#160; &#160;&#160; Canary Islands<br>11 June 2020&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160;&#160; Australia, CHEOPS satellite<br>27 August 2021 &#160; &#160; &#160; Australia</p><p>These campaigns were undertaken in a context where rings are already known to exists around other small bodies of the solar system: the Centaur object Chariklo [Br14] and the dwarf planet Haumea [Or17]. These two ring systems, in spite of large differences in sizes and heliocentric distances, both orbit close to the 1/3 Spin-Orbit Resonance (SOR) with the central body [Or17,Le17], meaning that the latter completes three rotations while a ring particle completes one orbital revolution. Because of their non-axisymmetric shapes, and contrarily to giant planets, Chariklo and Haumea induce strong SORs [Si19]. Theoretical calculations [Si21] and numerical simulations of collisional disks [Sa21] show that the 1/3 SOR is indeed a possible cause of confinement of a narrow ring.</p><p>If ring exists at the Quaoar 1/3 SOR, it should be close to an orbital radius of 4,200 km. This represents 7.5 Quaoar's radii, well outside the Roche limit of the central body. So, if a dense ring were to be confined near this resonance, it is expected to accrete into a satellite, and thus disappear over a short time scale. We will discuss models that could maintain a colliding disk near the Quaoar 1/3 SOR in spite of this obstacle.</p><p>Acknowledgments. The work leading to these results has received funding from the European Research Council under the European Community's H2020 2014-2021 ERC Grant Agreement no. 669416 "Lucky Star"</p><p>[Br13] Braga-Ribas et al., ApJ 773, 26 (2013)<br>[Fr10] Fraser and Brown, ApJ, 714, 1547 (2010)<br>[Le17] Leiva et al., Astron. J. 154, 159 (2017)<br>[Or17] Ortiz et al., Nature 550, 219 (2017)<br>[Sa21] Salo, H. et al., European Planetary Science Congress, EPSC2021-338 (2021)<br>[Si19] Sicardy, B. et al., Nature Astronomy 3, 146 (2019)<br>[Si21] Sicardy, B. et al., European Planetary Science Congress, EPSC2021-91 (2021)</p>
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hal-03835330 , version 1 (31-10-2022)

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Bruno Sicardy, Bruno Morgado, Felipe Braga-Ribas, Jose Luis Ortiz, Josselin Desmars, et al.. Search for rings around the large Trans-Neptunian Object (50000) Quaoar . Europlanet Science Congress 2022, Sep 2022, Granada, Spain. ⟨10.5194/epsc2022-82⟩. ⟨hal-03835330⟩
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