Size and Shape of Chariklo from Multi-epoch Stellar Occultations

DOI: 
10.3847/1538-3881/aa8956
Publication date: 
01/10/2017
Main author: 
Leiva, R.
IAA authors: 
Ortiz, J. -L.;Duffard, R.;Morales, N.
Authors: 
Leiva, R.;Sicardy, B.;Camargo, J. I. B.;Ortiz, J. -L.;Desmars, J.;Bérard, D.;Lellouch, E.;Meza, E.;Kervella, P.;Snodgrass, C.;Duffard, R.;Morales, N.;Gomes-Júnior, A. R.;Benedetti-Rossi, G.;Vieira-Martins, R.;Braga-Ribas, F.;Assafin, M.;Morgado, B. E.;Colas, F.;De Witt, C.;Sickafoose, A. A.;Breytenbach, H.;Dauvergne, J. -L.;Schoenau, P.;Maquet, L.;Bath, K. -L.;Bode, H. -J.;Cool, A.;Lade, B.;Kerr, S.;Herald, D.
Journal: 
The Astronomical Journal
Refereed: 
Yes
Publication type: 
Article
Volume: 
154
Pages: 
159
Abstract: 

We use data from five stellar occultations observed between 2013 and 2016 to constrain Chariklo’s size and shape, and the ring reflectivity. We consider four possible models for Chariklo (sphere, Maclaurin spheroid, triaxial ellipsoid, and Jacobi ellipsoid), and we use a Bayesian approach to estimate the corresponding parameters. The spherical model has a radius R = 129 ± 3 km. The Maclaurin model has equatorial and polar radii a=b={143}<SUB>-6</SUB><SUP>+3</SUP> {km} and c={96}<SUB>-4</SUB><SUP>+14</SUP> {km}, respectively, with density {970}<SUB>-180</SUB><SUP>+300</SUP> {kg} {{{m}}}<SUP>-3</SUP>. The ellipsoidal model has semiaxes a={148}<SUB>-4</SUB><SUP>+6</SUP> {km}, b={132}<SUB>-5</SUB><SUP>+6</SUP> {km}, and c={102}<SUB>-8</SUB><SUP>+10</SUP> {km}. Finally, the Jacobi model has semiaxes a = 157 ± 4 km, b = 139 ± 4 km, and c = 86 ± 1 km, and density {796}<SUB>-4</SUB><SUP>+2</SUP> {kg} {{{m}}}<SUP>-3</SUP>. Depending on the model, we obtain topographic features of 6─11 km, typical of Saturn icy satellites with similar size and density. We constrain Chariklo’s geometric albedo between 3.1% (sphere) and 4.9% (ellipsoid), while the ring I/F reflectivity is less constrained between 0.6% (Jacobi) and 8.9% (sphere). The ellipsoid model explains both the optical light curve and the long-term photometry variation of the system, giving a plausible value for the geometric albedo of the ring particles of 10%─15%. The derived mass of Chariklo of 6─8 × 10<SUP>18</SUP> kg places the rings close to 3:1 resonance between the ring mean motion and Chariklo’s rotation period. Based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia, e Inovação (MCTI) da República Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU).

Database: 
ADS
SCOPUS
URL: 
https://www.scopus.com/inward/record.uri?eid=2-s2.0-85031114679&doi=10.3847%2f1538-3881%2faa8956&partnerID=40&md5=67732a97bce2c4285cddef58db32f479
ADS Bibcode: 
2017AJ....154..159L
Keywords: 
methods: statistical;minor planets;asteroids: individual: Chariklo;occultations;planets and satellites: rings;Astrophysics - Earth and Planetary Astrophysics