The orbit, mass, and albedo of transneptunian binary (66652) 1999 RZ253

Noll, K. S.; Stephens, Denise C.; Grundy, W. M.; Griffin, I. P.

doi:10.1016/j.icarus.2004.06.009

Cited by 30 publications

(21 citation statements)

References 12 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Orbits for P1 and P2 about the Olkin et al (2003) barycenter were fitted using a downhill simplex minimization scheme ( Nelder & Mead 1965), using code developed for fitting orbits of binary transneptunian objects (Noll et al 2004a(Noll et al , 2004b. Initial results from these fits looked very promising, with residuals mostly at or below a single HRC pixel (0B025).…”

Section: Discussionmentioning

confidence: 99%

Orbits and Photometry of Pluto's Satellites: Charon, S/2005 P1, and S/2005 P2

et al. 2006

View full text Add to dashboard Cite

We present new astrometry of Pluto's three satellites from images taken of the Pluto system during [2002][2003] with the High Resolution Camera mode of the Advanced Camera for Surveys instrument on the Hubble Space Telescope. The observations were designed to produce an albedo map of Pluto, but they also contain images of Charon and the two recently discovered satellites S/2005 P1 and S/2005 P2. Orbits fitted to all three satellites are nearly coplanar and for Charon and P2 have eccentricities consistent with zero. The orbit of the outermost satellite, P1, has a significant eccentricity of 0:0052 AE 0:0011. Orbital periods of P1, P2, and Charon are 38:2065 AE 0:0014, 24:8562 AE 00013, and 6:3872304 AE 0:0000011 days, respectively. The total system mass based on Charon's orbit is 1:4570 AE 0:0009 ð Þ ; 10 22 kg. We confirm previous results that orbital periods are close to the ratio of 6 : 4 : 1 (P1 : P2 : Charon), indicative of mean-motion resonances, but our results formally preclude precise integer period ratios. The orbits of P1 and P2, being about the barycenter rather than Pluto, enable us to measure the Charon-to-Pluto mass ratio as 0:1165 AE 0:0055. This new mass ratio implies a density of 1:65 AE 0:06 g cm À3 for Charon (603.6 km radius) and 2:03 AE 0:06 g cm À3 for Pluto (1153 km radius), thus adding confirmation that Charon is significantly less dense than Pluto. Finally, by stacking all images we can extract globally averaged photometry. P1 has a mean opposition magnitude of V ¼ 24:39 AE 0:09 and a color of (B À V ) ¼ 0:64 AE 0:12. P2 has a mean opposition magnitude of V ¼ 24:55 AE 0:10 and a color of (B À V ) ¼ 0:91 AE 0:15.

show abstract

Section: Discussionmentioning

confidence: 99%

Orbits and Photometry of Pluto's Satellites: Charon, S/2005 P1, and S/2005 P2

et al. 2006

View full text Add to dashboard Cite

show abstract

“…In this case, several orbits with identical likelihoods can be found, and the search ranges for the orbital parameters are manually set (Noll et al 2004). We added non-gravitational effects, such as the precessions of the lines of nodes due to an irregularly shaped primary, to the geometrical model developed by Descamps (2005), giving us the possibility of deriving an estimate of the dynamical J 2 of the triple asteroid system (87) Sylvia (Marchis et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Determination of binary asteroid orbits with a genetic-based algorithm

Vachier

Berthier

Marchis

2012

A&A

View full text Add to dashboard Cite

Aims. Over the past decade, discoveries of multiple and binary asteroid systems have played a significant role in our general understanding of small solar system bodies. Direct observations of satellites of asteroids are rare and difficult since they require the use of already over-subscribed facilities such as adaptive optics (AO) on large 8−10 m class telescopes and the Hubble Space Telescope (HST). The scarcity of data and the long temporal baseline of observations (up to 10 years) significantly complicate the determination of the mutual orbits of these systems. Methods. We implemented a new approach for determining the mutual orbits of directly-imaged multiple asteroids using a geneticbased algorithm. This approach was applied to several known binary asteroid systems (22 Kalliope, 3749 Balam, and 50 000 Quaoar) observed with AO systems and HST. This statistical method is fast enough to permit the search for an orbital solution across a large parameter space and without a priori information about the mutual orbit. Results. From 10 years of observation, we derived an orbital solution for Linus, companion of (22) Kalliope, with an accuracy close to the astrometric limit provided by the AO observations, assuming a purely Keplerian orbit. A search for non-Keplerian orbit confirmed that a J 2 ∼ 0 is the best-fitting solution. We show that the precession of the nodes could be detected without ambiguity, implying that Kalliope's primary may have an inhomogeneous internal structure. HST astrometric observations of Weywot, companion of the trans-Neptunian object (50 000) Quaoar, were used to derive its mass and its bulk density, which appears to be higher than the density of other TNOs. Finally, we derived a bundle of orbital solutions for (3749) Balam, with equally good fits, from the limited set of astrometric positions. They provide a realistic density between 1.3 and 3.7 g/cm 3 for this S-type asteroid.

show abstract

“…This eventually leads to binaries having similarly sized partners. However, this mechanism appears to lead to orbital properties (in particular, mutual orbit eccentricities) dissimilar to those actually observed (Astakhov et al 2005;Noll 2003;Noll et al 2004). A further capture scenario, chaos-assisted capture (CAC; Astakhov et al 2005;Lee et al 2007) supposes that two objects become caught up in very long living, yet ultimately unstable, chaotic orbits within their mutual Hill sphere.…”

Section: Introductionmentioning

confidence: 95%

A possible mechanism to explain the lack of binary asteroids among the Plutinos

Compère

Farrelly

Lemaître

et al. 2013

A&A

View full text Add to dashboard Cite

Context. Binary asteroids are common in the solar system, including in the Kuiper belt. However, there seems to be a marked disparity between the binary populations in the classical part of the Kuiper belt and the part of the belt in the 3:2 resonance with Neptune -i.e., the region inhabited by the Plutinos. In particular, binary Plutinos are extremely rare. Aims. We study the impact of the 3:2 resonance on the formation of Kuiper belt binaries, according to the Nice model, in order to explain such phenomenon. Methods. Numerical simulations are performed within the 2 + 2 body approximation (Sun/Neptune + binary partners). The MEGNO chaos indicator is used to map out regular and chaotic regions of phase space. Residence times of test (binary) particles within the Hill sphere are compared inside and outside of the 3:2 resonance. The effect of increasing the heliocentric eccentricity of the centre of mass of the binary system is studied. This is done because mean-motion resonances between a planet and an asteroid usually have the effect of increasing the eccentricity of the asteroid. Results. The stable zones in the MEGNO maps are mainly disrupted in the resonant, eccentric case: the number of binary asteroids created in this case is significantly lower than outside the 3:2 resonance. Conclusions. In the 2 + 2 body approximation, the pumping of the eccentricity of the centre of mass of a potential binary destabilises the formation of binaries. This may be a factor in explaining the scarcity of binaries in the Plutino population.

show abstract

The orbit, mass, and albedo of transneptunian binary (66652) 1999 RZ253

Cited by 30 publications

References 12 publications

Orbits and Photometry of Pluto's Satellites: Charon, S/2005 P1, and S/2005 P2

Orbits and Photometry of Pluto's Satellites: Charon, S/2005 P1, and S/2005 P2

Determination of binary asteroid orbits with a genetic-based algorithm

A possible mechanism to explain the lack of binary asteroids among the Plutinos

Contact Info

Product

Resources

About