2 Pallas
Encyclopedia : 2 : 2P : 2PA : 2 Pallas
| Orbital elements | |
|---|---|
| Eccentricity (orbit)>e | |
| Inclination>i | ° |
| Perihelion>q |
|
| Argument of perihelion>ω | ° |
| Semi-major axis>a | AU |
| Longitude of the ascending node>ω | ° |
| Aphelion>Q |
|
| Mean anomaly>M | ° |
| Orbital period>P | years |
| Mean motion>n | °/day |
| Time of perihelion passage>TP | |
Name
The asteroid is named after Pallas, the daughter of Triton and friend of Athena in Greek mythology. (There are several male characters of the same name in Greek mythology, but the first asteroids were invariably given female names.)According to the OED, the adjectival form of Pallas is Palladian.
Characteristics
Pallas is the third largest asteroid, similar to 4 Vesta in volume (to within uncertainty), but significantly less massive.
Pallas is currently the largest Solar System body (barring trans-Neptunian objects) whose surface has not been directly imaged by spacecraft or telescopes. It may also be the largest irregularly-shaped body, meaning that it has not been compressed by gravity into a spheroid shape (other candidates may be trans-Neptunian objects such as 2003 EL61).
Pallas also has unusual dynamical parameters for such a large body. Its orbit is highly inclined and somewhat eccentric despite being located at the same distance from the sun as the central part of the Main belt.
Furthermore, its axial tilt is very high, being around 60° (in fact estimates vary from 56° to 81°) [4][7][9]. This means that, every palladian summer and winter, large parts of the surface are in constant sunlight or constant darkness for a time of the order of an Earth year. Consensus has not been reached as to whether Pallas' rotation is prograde or retrograde. The most recent analysis of lightcurves indicates that the pole points towards ecliptic coordinates (β, λ) = (-12°, 35°) or (43°, 193°) with a 10° uncertainty [9]. This gives axial tilts of 57° or 65°, respectively.
There are indications that the surface composition of Pallas is very similar to the Renazzo carbonaceous chondrite (CR) meteorites [8].
Observations
Some notable observation milestones for Pallas include:Pallas has been observed occulting a star several times, including the best observed of all asteroid occultation events on May 29, 1983, when careful occultation timing measurements were taken by 140 observers. These have helped determine an accurate diameter [5]. During the occultation of May 29, 1979 the discovery of a possible tiny satellite with a diameter of ~1 km was reported. However, it has not been confirmed. In 1980, speckle interferometry was reported as indicating a much larger satellite with a diameter of 175 km, but the existence of the satellite was later refuted. [link]
Radar signals from spacecraft in orbit around Mars and/or on its surface have been used to estimate the mass of Pallas from the tiny perturbations induced by it onto the motion of Mars [1].
There have not been any telescopic observations of Pallas that have resolved any features on its disk. Pallas has not yet been visited by a spacecraft, but if the Dawn probe is successful in studying 1 Ceres and 4 Vesta, its mission may be extended to Pallas.
Trivia
The chemical element palladium (atomic number 46) was named after Pallas.Aspects
A table with the aspects (opposition, conjunction to sun, etc.) of 2 Pallas from 2005 to 2020.
External links
References
- [E. V. Pitjeva, Estimations of Masses of the Largest Asteroids and the Main Asteroid Belt From Ranging to Planets, Mars Orbiters And Landers] Solar System Resarch, Vol. 39 pp. 176 (2005).
- [Supplemental IRAS Minor Planet Survey]
- [Other Reports of Asteroid Companions, compiled by Wm. Robert Johnston]
- J. D. Drummond and W. J. Cocke Triaxial ellipsoid dimensions and rotational pole of 2 Pallas from two stellar occultations, Icarus, Vol. 78, pp. 323 (1989).
- [D. W. Dunham et al The size and shape of (2) Pallas from the 1983 occultation of 1 Vulpeculae], The Astronomical Journal, Vol. 99, pp. 1636 (1990).
- [E. Goffin New determination of the mass of (2) Pallas], Astronomy and Astrophysics, Vol. 365, pp. 627 (2001).
- D. L. Mitchell et al Radar observations of asteroids 1 Ceres, 2 Pallas, and 4 Vesta, Icarus, Vol. 124, pp. 113 (1996).
- [Sato et al Absorption bands near three micrometers in diffuse reflectance spectra of carbonaceous chondrites: Comparison with asteroids], Meteoritics and Planetary Science, Vol. 32, pp. 503 (1997).
- [J. Torppa et al Shapes and rotational properties of thirty asteroids from photometric data], Icarus, Vol. 164, p. 346 (2003).
- [James L. Hilton, U.S. Naval Observatory Ephemerides of the Largest Asteroids] The Astronomical Journal, Vol. 117 pp. 1077 (1999).
See also
| The minor planets |
|---|
| Vulcanoids | Near-Earth asteroids | Main belt | Jupiter Trojans | Centaurs | Damocloids | Comets | Trans-Neptunians (Kuiper belt · Scattered disc · Oort cloud) |
| For other objects and regions, see: , , asteroid moons and the Solar system For a complete listing, see: List of asteroids. See also Pronunciation of asteroid names and Meanings of asteroid names. |
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