Size, density, albedo and atmosphere limit of dwarf planet Eris from a stellar occultation
English
Sicardy, B.[Instituto de Astrofisica de Andalucia, Spain]
Ortiz, J. L.[Observatorio do Valongo / UFRJ, Brazil]
Assafin, M.[Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astrophysique et traitement de l'image]
Jehin, Emmanuel[San Pedro de Atacama Celestial Explorations, Chile]
Maury, A.[Observatoire de Paris-Meudon, Meudon Cédex, France (bruno.sicardy@obspm.fr)]
Lellouch, E.[Complejo Astronomico El Leoncito and San Juan National University, Argentina]
Gil-Hutton, R.[Observatoire de Paris-Meudon, Meudon Cédex, France; Observatorio Nacional / MCT, Brazil]
Braga-Ribas, F.[Observatoire de Paris-Meudon, Meudon Cédex, France)]
Colas, F.[Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astrophysique et traitement de l'image]
Lecacheux, J.[Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Département d'astrophys., géophysique et océanographie (AGO)]
[en] We report the observation of a multi-chord stellar occultation by the dwarf planet (136199) Eris. The event was observed on November 6, 2010 UT, from two sites in Chile. Our observation is consistent with a spherical Eris with radius RE=1163±6 km, density =2.52±0.05 g cm-3, and visible geometric albedo pV=0.96+0.09 -0.04. Besides being remarkably similar in size to Pluto, Eris appears as one of the intrinsically brightest objects of the solar system, with a density suggesting a mainly rocky interior. Upper limits of about 1 nbar are derived for the surface pressure of possible nitrogen, argon or methane atmospheres of the dwarf planet.