Search arXiv⌕ Search
Home/Archive/arXiv

arXiv · 1706.00207

The structure of Chariklo's rings from stellar occultations

D. Bérard·B. Sicardy·J. I. B. Camargo·J. Desmars·F. Braga-Ribas·J. L. Ortiz·R. Duffard·N. Morales·E. Meza·R. Leiva·G. Benedetti-Rossi·R. Vieira-Martins·A. R. Gomes-Júnior·M. Assafin·F. Colas·J. L. Dauvergne·P. Kervella·J. Lecacheux·L. Maquet·F. Vachier·S. Renner·B. Monard·A. A. Sickafoose·H. Breytenbach·A. Genade·W. Beisker·K. L. Bath·H. J. Bode·M. Backes·V. D. Ivanov·E. Jehin·M. Gillon·J. Manfroid·J. Pollock·G. Tancredi·S. Roland·R. Salvo·L. Vanzi·D. Herald·D. Gault·S. Kerr·H. Pavlov·K. M. Hill·J. Bradshaw·M. A. Barry·A. Cool·B. Lade·A. Cole·J. Broughton·J. Newman·R. Horvart·D. Maybour·D. Giles·L. Davis·R. A. Paton·B. Loader·A. Pennell·P. D. Jaquiery·S. Brillant·F. Selman·C. Dumas·C. Herrera·G. Carraro·L. Monaco·A. Maury·A. Peyrot·J. P. Teng-Chuen-Yu·A. Richichi·P. Irawati·C. De Witt·P. Schoenau·R. Prager·C. Colazo·R. Melia·J. Spagnotto·A. Blain·S. Alonso·A Román·P. Santos-Sanz·J. L. Rizos·J. L. Maestre·D. Dunham
View original source ↗Read source document ↗Export metadata ↓

Abstract

Two narrow and dense rings (called C1R and C2R) were discovered around the Centaur object (10199) Chariklo during a stellar occultation observed on 2013 June 3. Following this discovery, we planned observations of several occultations by Chariklo's system in order to better characterize the physical properties of the ring and main body. Here, we use 12 successful occulations by Chariklo observed between 2014 and 2016. They provide ring profiles (physical width, opacity, edge structure) and constraints on the radii and pole position. Our new observations are currently consistent with the circular ring solution and pole position, to within the $\pm 3.3$ km formal uncertainty for the ring radii derived by Braga-Ribas et al. The six resolved C1R profiles reveal significant width variations from $\sim 5$ to 7.5 km. The width of the fainter ring C2R is less constrained, and may vary between 0.1 and 1 km. The inner and outer edges of C1R are consistent with infinitely sharp boundaries, with typical upper limits of one kilometer for the transition zone between the ring and empty space. No constraint on the sharpness of C2R's edges is available. A 1$σ$ upper limit of $\sim 20$ m is derived for the equivalent width of narrow (physical width <4 km) rings up to distances of 12,000 km, counted in the ring plane.

Explore related subjects

astro-ph.EP

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

D. Bérard, B. Sicardy, J. I. B. Camargo, J. Desmars, F. Braga-Ribas, J. L. Ortiz, R. Duffard, N. Morales, E. Meza, R. Leiva, G. Benedetti-Rossi, R. Vieira-Martins, A. R. Gomes-Júnior, M. Assafin, F. Colas, J. L. Dauvergne, P. Kervella, J. Lecacheux, L. Maquet, F. Vachier, S. Renner, B. Monard, A. A. Sickafoose, H. Breytenbach, A. Genade, W. Beisker, K. L. Bath, H. J. Bode, M. Backes, V. D. Ivanov, E. Jehin, M. Gillon, J. Manfroid, J. Pollock, G. Tancredi, S. Roland, R. Salvo, L. Vanzi, D. Herald, D. Gault, S. Kerr, H. Pavlov, K. M. Hill, J. Bradshaw, M. A. Barry, A. Cool, B. Lade, A. Cole, J. Broughton, J. Newman, R. Horvart, D. Maybour, D. Giles, L. Davis, R. A. Paton, B. Loader, A. Pennell, P. D. Jaquiery, S. Brillant, F. Selman, C. Dumas, C. Herrera, G. Carraro, L. Monaco, A. Maury, A. Peyrot, J. P. Teng-Chuen-Yu, A. Richichi, P. Irawati, C. De Witt, P. Schoenau, R. Prager, C. Colazo, R. Melia, J. Spagnotto, A. Blain, S. Alonso, A Román, P. Santos-Sanz, J. L. Rizos, J. L. Maestre, D. Dunham. 2017-09-18. The structure of Chariklo's rings from stellar occultations. https://doi.org/10.3847/1538-3881%2Faa830d

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

Volcanic Satellites and Ion Escape in the Magnetospheres of Ultra-Cool and Brown Dwarf Stars

Radio emissions at $\sim$ GHz frequencies of ultra-cool dwarf and brown dwarf stars suggest the presence of radiation belts not unlike Jupiter's. We investigate the possibility the inferred magnetospheric plasma at the primary star is sourced by an active planet or via ion escape modeled as a weak ionospheric outflow. We consider indirect methods to estimate the magnetospheric plasma mass flow from auroral radio emission and apply them to the ultra-cool dwarf LSR J1835+3259. We find that an ionospheric outflow is a viable source of the order of $10^{5}$ kg s$^{-1}$, if the ionospheric effective Pedersen conductance is lower than $\sim 0.02$ mho. On the other hand, a tidally-heated volcanic satellite with the same mass and radius as Io and an orbit with a semimajor axis lower than about $10$ stellar radii, whose eccentricity ($e \sim 10^{-3}$) is maintained by perturbations by other planets in the system, is found to be a viable source of magnetospheric plasma without strong limitations on the ionospheric conductance. The volcanic satellite scenario is also naturally in sync with the recent finding that ultra-cool dwarfs with distant substellar or stellar companions are remarkably more likely to be detected as radio emitters.

astro-ph.EP↗
arXiv2026

Tidal Demise: The Evolution and Fate of a Hypothetical Venus Moon

Venus possesses no natural satellite, raising the question whether a formed moon could have survived. We explore the tidal evolution of a Venus-moon system, coupling Venus's spin to the satellite's orbit under tides from the moon and Sun. We survey spin period ($P_0 = 5$--100~hr), moon mass ($M_m = 0.01$--$10~M_{\rm Moon}$), eccentricity, quality factor, and initial semi-major axis under both constant-$Q$ and constant time lag models. Survival depends on competition between outward migration ($\propto M_m$) and synchronous radius expansion ($\propto M_m^2$): for circular orbits around rapidly spinning Venus ($P_0 \lesssim 12$~hr), a lunar-mass satellite survives the age of the Solar System in both models. For $P_0 \lesssim 10$~hr, eccentricity pumping can destabilize low-mass satellites, while for $P_0 \gtrsim 15$~hr or $M_m \gtrsim 2~M_{\rm Moon}$ the synchronous radius overtakes the orbit and drives Roche destruction within $\sim$0.03--1.7~Gyr in the constant-$Q$ model. The constant time lag model instead permits quasi-synchronous survival for massive moons at fast spin. Explaining Venus's present state requires satisfying two constraints simultaneously: loss of the satellite and despinning of an initially rapid rotator. Both are met only within a restricted region of parameter space, favoring moderate post-impact spin periods and lunar-to-super-lunar masses. Giant impact simulations predict spin periods $\gtrsim$12~hr for Venus's present rotation, placing a lunar-mass satellite at the survival boundary. For last-impact conditions within this region, the present absence of a Venusian satellite arises through tidal evolution alone; a subsequent catastrophic stripping event, while capable of removing a moon, is not required.

astro-ph.EP↗
arXiv2026

Evidence for an Extended Hydrogen Outflow on WASP-12 b

Recent observations of atmospheric escape from planets orbiting early-type stars indicate that planets with higher Roche filling factors have significantly higher mass loss rates. For three of these planets, full-orbit observations have revealed the presence of large leading and trailing tails of escaping planetary material. These 3D outflow geometries encode information about the underlying outflow physics, and can also be used to constrain their stellar wind properties and to predict their long-term orbital evolution. We present new evidence for extended H$α$ and H$β$ absorption from escaping hydrogen for a fourth planet, WASP-12 b. We observed WASP-12 b with the Keck Planet Finder on Keck I over a period of approximately eight hours centered on the transit. We find a H$α$ and H$β$ absorption signal in the stellar rest frame that is strongest during the transit (H$α$ amplitude: $2.66\pm0.25\%$, H$β$ amplitude: $2.88\pm0.43\%$), with evidence of both pre- and post-transit absorption. This measurement is consistent with outflow models where the escaping gas overflows the planet's Roche lobe and is advected into the stellar rest frame before being tidally sheared into extended tails. This outflow behavior is qualitatively similar to previous H$α$ observations of this planet as well as observations of extended outflows from other gas giants orbiting early-type stars.

astro-ph.EP↗