Orbital and Physical Characterization of Centaur and TNO Binaries

Details Orbital and Physical Characterization of Centaur and TNO Binaries Orbital and Physical Characterization of Centaur and TNO Binaries

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.4417f&link_type=abstract

American Astronomical Society, DPS meeting #38, #44.17; Bulletin of the American Astronomical Society, Vol. 38, p.1300

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Scientific paper

A significant proportion of transneptunian objects are binaries [1] and their orbital properties and size ratios seem to agree with recent theoretical predictions [2]. Knowing the orbits of gravitionally bound binaries (or multiples) allows a direct and accurate determination of their total mass. This paves the way to determine other properties, e.g., bulk density, mass distribution, etc.
However, transneptunian resolved (or visual) binaries are often difficult to observe even with the largest ground-based telescopes; these systems can, however, be significantly better characterized with the HST HR Camera.
Orbit determination can also be enhanced using an algorithm we have developed [3] using techniques based on [4]: here we illustrate this method for binary true orbit inclinations (in addition to other orbital parameters) for the following reasons:
1. to test formation models which predict that prograde and retrogade mutual orbits will not be symmetrically distributed.
2. to provide accurate predictions of stellar occultations and extremely rare mutual phenomena (eclipses/occultations). Observations in the infra-red will allow the thermal inertia of the surface of each component to be determined.
3. spectroscopy and colorimetry of individually resolved components will shed light on the origins (collisional or capture) of binary and multiplet objects and provide constraints on relative physical composition.
Here, aspects of the orbit determination of resolved Centaur and transneptunian binaries are discussed with possible application to astrometric binaries. Estimates are obtained in terms of p.d.f.s of orbital parameters and consequently the total mass. This approach provides ranges of plausible bulk densities to be compared to surface compositions obtained spectroscopically.
[1] Noll K., 2006, TNO06 workshop, July 2006 Catania, Italy.
[2] Astakhov S.A., Lee, E. A., Farrelly. D., 2005, MNRAS 360, 401.
[3] Hestroffer D., Vachier F., Balat B., 2006, EM&P, in press.
[4] Virtanen J., Muinonen K., Bowell E., 2001, Icarus 154, 412.

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