Satellites of the Largest Kuiper Belt Objects

Brown, Michael E.; Dam, Marcos A. van; Bouchez, Antonin H.; Mignant, D. Le; Campbell, Randy; Chin, Jason C. Y.; Conrad, Al; Hartman, Scott; Johansson, Erik M. J.; Lafon, Robert E.; Rabinowitz, D.; Stomski, Paul J.; Summers, Douglas M.; Trujillo, C. A.; Wizinowich, Peter

doi:10.1086/501524

Cited by 139 publications

(157 citation statements)

References 12 publications

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“…The largest has a 50 day orbit and a measured orbital eccentricity of 0.050 ± 0.003 (Brown et al 2005). An additional smaller satellite orbits 2003 EL 61 with a period of about 35 days (Brown et al 2006). With these parameters we use Equation (23) to calculate an equilibrium e c = 4.3 × 10 −4 .…”

Section: Other Interesting Kbosmentioning

confidence: 99%

Lévy Flights of Binary Orbits Due to Impulsive Encounters

Collins¹,

Sari²

2008

The Astronomical Journal

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We examine the evolution of an almost-circular Keplerian orbit interacting with unbound perturbers. We calculate the change in eccentricity and angular momentum that results from a single encounter, assuming that the timescale for the interaction is shorter than the orbital period. The orbital perturbations are incorporated into a Boltzmann equation that allows for eccentricity dissipation. We present an analytic solution to the Boltzmann equation that describes the distribution of orbital eccentricity and relative inclination as a function of time. The eccentricity and inclination of the binary do not evolve according to a normal random walk but perform a Lévy flight. The slope of the mass spectrum of perturbers dictates whether close gravitational scatterings are more important than distant tidal ones. When close scatterings are important, the mass spectrum sets the slope of the eccentricity and inclination distribution functions. We use this general framework to understand the eccentricities of several Kuiper belt systems: Pluto, 2003 EL 61 , and Eris. We use the model of Tholen et al. to separate the non-Keplerian components of the orbits of Pluto's outer moons Nix and Hydra from the motion excited by interactions with other Kuiper belt objects. Our distribution is consistent with the observations of Nix, Hydra, and the satellites of 2003 EL 61 and Eris. We address applications of this work to objects outside of the solar system, such as extra-solar planets around their stars and millisecond pulsars.

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Section: Other Interesting Kbosmentioning

confidence: 99%

Lévy Flights of Binary Orbits Due to Impulsive Encounters

Collins¹,

Sari²

2008

The Astronomical Journal

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“…This object, recently baptized "Eris" (IAU 2006), revealed a number of features in common with Pluto, despite being a member of the family of the scattered TNO (Sheppard 2006). As an example, like Pluto, Eris has a satellite named "Dysnomea" with an orbital period of about two weeks, a brightness of about 2% of that of Eris, and a semi-major axis of ≈5 × 10 4 km (Brown et al, 2006a). Eris' IR spectrum is clearly dominated by CH 4 absorption bands (Brown et al, 2006b) and perhaps shows N 2 bands (Licandro et al, 2006).…”

Section: Introductionmentioning

confidence: 98%

Time series photometry of the dwarf planet ERIS (2003 UB313)

Carraro

Maris

Bertin

et al. 2006

A&A

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Context. The dwarf planet Eris (2003 UB313, formerly known also as "Xena") is the largest KBO discovered up to now. Despite being larger than Pluto and having many similarities to it, it has not been possible so far to detect any significant variability in its light curve, preventing the determination of its period and axial ratio. Aims. We attempt to assess the level of variability of the Eris light curve by determining its BVRI photometry with a target accuracy of 0.03 mag/frame in R and a comparable or better stability in the calibration. This cannot be explained by known systematics, background objects, or some periodical variation with periods less than two days in the lightcurve. The same applies to B, V and to a lesser extent to I, due to larger errors. Conclusions. In analogy with Pluto and if confirmed by future observations, this "long term" variability might be ascribed to a slow rotation of Eris, with periods longer than 5 days, or to the effect of its unresolved satellite "Dysnomea", which may contribute for ≈0.02 mag to the total brightness.

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“…Brown et al (2006b), using the Hubble Space Telescope directly measured the size of Eris and determine a diameter of (2400 ± 100) km or a size 5% larger than Pluto. Bertoldi et al (2006) measured the thermal emission of Eris at a wavelength of 1.2 mm, and combined their observations with the measured optical brightness, leading to a diameter of (3000 ± 300) km.…”

Section: Introductionmentioning

confidence: 99%

“…Adaptive optics observations of Eris at the Keck telescopes in Hawaii revealed a moon, called Dysnomia, in orbit around Eris (Brown et al 2006b). The discovery of the satellite presented the opportunity to measure the mass of Eris.…”

Section: Introductionmentioning

confidence: 99%

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A study of photometric variations on the dwarf planet (136199) Eris

Duffárd

Ortiz

Santos-Sanz

et al. 2007

A&A

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Context. Eris is the largest dwarf planet currently known in the solar system. Knowledge about its physical parameters is necessary to interpret the characteristics of these kinds of bodies. Aims. The goal of this work is to study Eris' short-term and long-term variability in order to determine the amplitude of the lightcurve, which can be linked to the degree of elongation of the body or to the degree of albedo heterogeneity on the surface of the dwarf planet. In addition, the rotation period can be determined. Methods. CCD photometric observations of the trans Neptunian object Eris in R band on 16 nights spanning two years were carried out using the 1.5 m telescope at Sierra Nevada Observatory (OSN), the 2.5 m Isaac Newton Telescope (INT) telescope at the Roque de los Muchachos Observatory, and the 2.2 m Telescope at Calar Alto Observatory. Results. The time-series analysis leads to indications of a short-term variability whose nature is not clear. It could be real or a result of data-reduction artifacts, such as contamination by close, faint-background stars. The most significant periodicities are 14 h or its double, but other possibilities cannot be ruled out, like a 32 h weaker peak in the periodogram. As for the amplitude of the lightcurve, we get a peak-to-peak variability of 0.01 ± 0.01 mag. The study of the long-term variability indicates that a long rotation period cannot be rejected, but the amplitude would be smaller than 0.06 mag. These results are compatible with a nearly spherical body that has a homogeneous surface.

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Satellites of the Largest Kuiper Belt Objects

Cited by 139 publications

References 12 publications

Lévy Flights of Binary Orbits Due to Impulsive Encounters

Lévy Flights of Binary Orbits Due to Impulsive Encounters

Time series photometry of the dwarf planet ERIS (2003 UB313)

A study of photometric variations on the dwarf planet (136199) Eris

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