Charon/Pluto Mass Ratio Obtained with HST CCD Observations in 1991 and 1993

Null, G. W.; M., Jr. Owen W.

doi:10.1086/117883

Cited by 21 publications

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“…In Table 1 a chronology of mass ratios μ = mC/mP and mass parameters µ = mC/(mP + mC) is shown, where mP and mC are the masses of Pluto and Charon, respectively. Several authors have struggled to obtain this quantity from measurements of the barycentric wobble (Null et al 1993;Young & Binzel 1994;Null & Owen 1996;Tholen & Buie 1997;Foust et al 1997;Olkin et al 2003). In addition the Pluto-Charon system is remarkable, since in the Solar system Charon is the largest moon relative to its primary, with the highest mass ratio of 0.1166 (Tholen et al 2008) (hereafter referenced to as T08).…”

Section: Introductionmentioning

confidence: 99%

“…In the first six rows values derived form the barycentric wobble are listed, while in the last two rows those calculated from orbital fits using the discovery of the small moons. Young & Binzel (1994) 1.566 ± 3.50e − 3 1.3540 +2.608e−3 −2.624e−3 Null & Owen (1996) 1.240 ± 8.00e − 3 1.1032 +6.287e−3 −6.378e−3 Tholen & Buie (1997) 1.100 ± 6.00e − 2 0.9910 +4.620e−2 −5.148e−2 Foust et al (1997) 1.170 ± 6.00e − 3 1.0474 +4.783e−3 −4.835e−3 Olkin et al (2003) 1.220 ± 8.00e − 3 1.0873 +6.310e−3 −6.400e−3 Buie et al (2006) 1.165 ± 5.50e − 3 1.0434 +4.390e−3 −4.434e−3 Tholen et al (2008) 1.166 ± 6.90e − 3 1.0442 +5.500e−3 −5.569e−3 Mean 1.1183 1.05537 the mass ratios and mass parameters are given in the last row of Table 1. In the works of Buie et al (2006) (hereafter referenced to as B06) and T08 the masses were derived from two-body and fourbody fits, respectively.…”

Section: Introductionmentioning

confidence: 99%

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Detailed survey of the phase space around Nix and Hydra

Süli

Zsigmond

2009

Monthly Notices of the Royal Astronomical Society

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We present a detailed survey of the dynamical structure of the phase space around the new moons of the Pluto - Charon system. The spatial elliptic restricted three-body problem was used as model and stability maps were created by chaos indicators. The orbital elements of the moons are in the stable domain both on the semimajor axis - eccentricity and - inclination spaces. The structures related to the 4:1 and 6:1 mean motion resonances are clearly visible on the maps. They do not contain the positions of the moons, confirming previous studies. We showed the possibility that Nix might be in the 4:1 resonance if its argument of pericenter or longitude of node falls in a certain range. The results strongly suggest that Hydra is not in the 6:1 resonance for arbitrary values of the argument of pericenter or longitude of node.Comment: Published in MNRAS. 10 pages, 7 figures, 4 table

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Detailed survey of the phase space around Nix and Hydra

Süli

Zsigmond

2009

Monthly Notices of the Royal Astronomical Society

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“…With greater attention to achieving the best possible seeing, some direct imaging observations now compete with HST. The bulk density of Charon has been measured both from HST and from the ground, showing that Charon has a lower density than Pluto (Null et al 1993, Young et al 1994, Null and Owen 1996. Even newer techniques based on adaptive optics on the largest telescopes are also being turned toward imaging, photometric, and spectroscopic investigations.…”

Section: Introductionmentioning

confidence: 99%

The Distribution and Physical State of H2O on Charon

Buie

Grundy

2000

Icarus

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“…Estimates for a vary between 19,405 km and 19,662 km [Null et aI., 1993;Null and Owen, 1996], while the estimates ofR e range from 1 I00 km to 1206 km [McKinnon et al, 1997, p. 298]. The measurements based on mutual events and direct imaging, which appear to give the most accurate results, put R e between about I 150 km and 1200 kin; this is the range which will be adopted here.…”

Section: Pluto's Precessionmentioning

confidence: 99%

Pluto and Charon: A case of precession‐orbit resonance?

Rubincam

2000

J. Geophys. Res.

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Pluto may be the only known case of precession‐orbit resonance in the solar system. The Pluto‐Charon system orbits the Sun with a period of 1 Plutonian year, which is 250.8 Earth years. The observed parameters of the system are such that Charon may cause Pluto to precess with a period near 250.8 Earth years. This gives rise to two possible resonances, heretofore unrecognized. The first is due to Pluto's orbit being highly eccentric, giving solar torques on Charon with a period of 1 Plutonian year. Charon, in turn, drives Pluto near its precession period. Volatiles, which are expected to shuttle across Pluto's surface between equator and pole as the insolation varies, might change the planet's dynamical flattening enough so that Pluto crosses the nearby resonance, forcing the planet's equatorial plane to depart from Charon's orbital plane. The mutual tilt can reach as much as 3° after integrating over 8.4×106 years, depending upon how close Pluto is to the resonance and the supply of volatiles. The second resonance is due to the Sun's traveling above and below Charon's orbital plane; it has a period half that of the eccentricity resonance. Reaching this half‐Plutonian‐year resonance requires a much larger but still theoretically possible amount of volatiles. In this case the departure of Charon from an equatorial orbit is ∼1° after integrating for 5.6×106 years. The calculations ignore libration and tidal friction. It is not presently known how large the mutual tilt can grow over the age of the solar system, but it is probably less than ∼4°. If so, then observing such small angles from a Pluto flyby mission would be difficult.

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Charon/Pluto Mass Ratio Obtained with HST CCD Observations in 1991 and 1993

Cited by 21 publications

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Detailed survey of the phase space around Nix and Hydra

Detailed survey of the phase space around Nix and Hydra

The Distribution and Physical State of H2O on Charon

Pluto and Charon: A case of precession‐orbit resonance?

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