Accès ouvert déclaré
2026
preprint
Size, shape, density, and atmospheric limit of (50000) Quaoar revealed from 14 years of stellar occultation
G. Margoti, F. Braga-Ribas, J Ortiz, Bruno Sicardy, Josselin Desmars, B. E. Morgado, Eros de Oliveira Gradovski, C. L. Pereira, Pablo Santos-Sanz, Altair Ramos Gomes-Júnior, Julio Ignacio Bueno de Camargo, M. Assafin, Vieira-Martins Roberto, Yucel Kilic, D. Souami, René Duffard, Gustavo Benedetti-Rossi, Tiago Pinheiro, Maísa Poiani, Eduardo Rondón, M Di Paolo Emilio, D. Herald, Rafael Sfair, Nicolas Morales, Francois Colas, F. Vachier, Mónica Vara Lubiano, Rodrigo Boufleur, Mert Acar, Francisco J. Aceituno, Miguel R. Alarcon, Sinan Alis, Sergio Alonso, J. Alonso-Santiago, Flavia Amadio, Laerte Andrade, P André, Jonatã Arcas-Silva, Alper K. Ateş, David Lafuente Aznar, Michael Backes, M. N. Bagiran, Nelson Balcar, M. A. Barry, K Barkaoui, W. Beisker, Kirk Bender, Zouhair Benkhaldoun, Svetlana Boeva, Eberhard H. R. Bredner, Richard Busuttil, A. ~Y. ~Burdanov, Oscar Canales, Javier Zaragoza-Cardiel, V. Casanova, Matheus Leal Castanheira, Peter Ceravolo, Steven J. Conard, Luciano Negrello Correa, Daniel V. Cotton, V S Dhillon, Serena Diamond, Vlad Dumitrescu, Joan Dunham, David W. Dunham, Christopher L. Duston, Eslam Elhosseiny, O. Erece, Sila Eryilmaz, Emilio J. Fernández-García, Süleyman Fişek, R. S. Fisher, Clyde Foster, Eric Frappa, Antonio Frasca, J I Frey, José María Gómez-Limón Gallard, Jose Luis Maestre Garcia, D. Gault, Kosmas Gazeas, Kai Getrost, M Gillon, Alan Gilmore, Robert Glassey, K. D. Green, William Hanna, Nicholas J. Haigh, Dean Hooper, Kamil Hornoch, D. Ilić, C. Jacques, Felix~Jankowsky, Emmanuel Jehin, S. Kalkan, Roxanne Kamin, Monika K. Kaminska, Shai Kaspi, J. J. Kavelaars, Stephen Kerr, Ulrich Kolb, Richard Komvzik, Dogan T. Koseoglu, M. Kretlow, Sangeeta Kuchibhotla, Jean Lecacheux, A. Leroy, A. Liakos, L. Liberato, Peter Lindner, S. P. Littlefair, José M. Madiedo, Natalio Maicas, Marcio Malacarne, Paul Maley, J. Manek, A. Marciniak, Patrick Martínez, R. Iglesias-Marzoa, Graeme McKay, S. Messner, Z. Moravec, Eduardo Fonseca Morato, Messias Fidêncio Neto, J Newman, V. Nikitin, Richard Nolthenius, Peter Nosworthy, Mohammad Odeh, W. Ogloza, Sibel Ötken, Sacit Özdemir, A Pal, Ashley Pennell, Amauri Pereira, Carles Perelló, Jean Perkins, Konstantin von Poschinger, Thiago do Prado, T. Pribulla, S. Rahvar, Giovana Ramon, Seth Redfield, C. Rinner, Jean‐Pierre Rivet, Johannes Antunes Nascimento Ro, rigues Antonio Román-Reche, F. L. Rommel, T. Santana, T. Santana-Ros, Antoni Selva, Christoph M. Schaefer, Andrew Scheck, Carles Schnabel, Olivier Schreurs, Andreas Schweizer, M Serra-Ricart, Ned Smith, Colin Snodgrass, Э. Сонбас, A. Sota, Rafael Ribeiro de Sousa, Fábio Augusto Spina, Theodore Swift, Róbert Szakáts, A. Takey, Mohammad F. Talafha, R. Teixeira, Z. Terzioğlu, Qiushi Tian, Vagelis Tsamis, Eyüp Kaan ÜLGEN, O. Vince, Marcos Rincón Voelzke, Christian Weber, J de Wit, Michal Zejmo
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Résumé fourni par la source
We present results from 28 stellar occultations by the large Trans-Neptunian Object (50000) Quaoar registered between 2018 and 2025. By performing a joint analysis of this occultation data-set, along with other 9 published events, we were able to fit an oblate ellipsoid shape, with equatorial semi-axes, a and b of 566.1+2.5-2.2 km, and a polar semi-axis, c, of 511.2+3.6-3.7 km. It provides an equivalent volumetric diameter of 1094.4 +/- 4.6 km and polar oblateness of 0.097 +/- 0.011. Considering an absolute magnitude of H = 2.79 +/- 0.35, we derive a geometric albedo of pV = 0.125 +/- 0.038. We have derived new upper limits to the surface pressure of a CH4 atmosphere of 0.15 nbar (1-sigma) and 0.65 nbar (3-sigma). We also provide a table with the 36 new astrometric positions for Quaoar. Using the new system mass derived from Weywot's orbit around Quaoar, we calculated a density of 1.760 +/- 0.109 g/cm3. Moreover, from the derived size and rotation period (8.8394 +/- 0.0002 hours (Ortiz et al. 2003)), we calculate that, if Quaoar is in Maclaurin hydrostatic equilibrium state, it would have a density of 1.859 +/- 0.200 g/cm3. This result, within the error bars, is compatible with the value we found. Therefore, this work shows that Quaoar can be a Maclaurin object, being eligible as a dwarf planet.
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Sujets associés
Astro and Planetary ScienceStellar, planetary, and galactic studiesAstrophysics and Star Formation Studies