|Discovered by||Heinrich Wilhelm Olbers|
|Discovery date||March 28, 1802|
|Epoch 2014-Dec-09 (JD 2457000.5)|
|Aphelion||3.412605509 AU (510.4 Gm)|
|Perihelion||2.13060671 AU (318.9 Gm)|
|2.77160611 AU (414.7 Gm)|
|4.614296176 a (1685.371678 d)|
Average orbital speed
|Inclination||34.840998° to Ecliptic
34.21° to Invariable plane
|Proper orbital elements|
Proper semi-major axis
Proper mean motion
|78.041654 deg / yr|
Proper orbital period
Precession of perihelion
|-1.335344 arcsec / yr|
Precession of the ascending node
|−46.393342 arcsec / yr|
|Dimensions||582 × 556 × 500±18 km
544 km (mean)
|≈ 2.8 g/cm³|
|≈ 0.18 m/s² / .018g|
|≈ 0.32 km/s|
Equatorial rotation velocity
|likely 78°±13° |
|Temperature||≈ 164 K
max: ≈ 265 K (−8 °C)
|6.49 to 10.65|
|0.629″ to 0.171″|
Pallas, minor-planet designation 2 Pallas, is the second asteroid to have been discovered (after Ceres), and it is one of the largest asteroids in the Solar System. It is estimated to comprise 7% of the mass of the asteroid belt, and its diameter of 544 kilometres (338 mi) is slightly larger than that of 4 Vesta. It is 10–30% less massive than Vesta, placing it third among the asteroids. It is likely a remnant protoplanet.
When Pallas was discovered by astronomer Heinrich Wilhelm Matthäus Olbers on March 28, 1802, it was counted as a planet, as were other asteroids in the early 19th century. The discovery of many more asteroids after 1845 eventually led to their reclassification.
The Palladian surface appears to be a silicate material; the surface spectrum and estimated density resemble carbonaceous chondrite meteorites. The Palladian orbit, at 34.8°, is unusually highly inclined to the plane of the asteroid belt, and the orbital eccentricity is nearly as large as that of Pluto, making Pallas relatively inaccessible to spacecraft.[a]
2 Pallas is named after Pallas Athena (Ancient Greek: Παλλάς Ἀθηνᾶ), an alternate name for the goddess Athena. In some mythologies Athena killed Pallas, then adopted her friend's name out of mourning. (There are several male characters of the same name in Greek mythology, but the first asteroids were invariably given female names.)
Pallas is a Greek name and some other languages use variant versions of it for the asteroid: in Italian, Pallade, Russian Pallada, Spanish Palas, and Arabic Bālās, for example. In Chinese, however, the asteroid has a different name, 智神星 zhìshénxīng (which means "the wisdom-god(dess) star"), even though the Chinese call the goddess Pallas herself by the Greek name (帕拉斯 pàlāsī).
The stony-iron Pallasite meteorites are not connected to the Pallas asteroid, being instead named after the German naturalist Peter Simon Pallas. The chemical element palladium, on the other hand, was named after the asteroid, which had been discovered just before the element.
History of observation
In 1801, the astronomer Giuseppe Piazzi discovered an object which he initially believed to be a comet. Shortly thereafter he announced his observations of this object, noting that the slow, uniform motion was uncharacteristic of a comet, suggesting it was a different type of object. This was lost from sight for several months, but was recovered later in the year by the Baron von Zach and Heinrich W. M. Olbers after a preliminary orbit was computed by Friedrich Gauss. This object came to be named Ceres, and was the first asteroid to be discovered.
A few months later, Olbers was again attempting to locate Ceres when he noticed another moving object in the vicinity. This was the asteroid Pallas, coincidentally passing near Ceres at the time. The discovery of this object created interest in the astronomy community. Before this point it had been speculated by astronomers that there should be a planet in the gap between Mars and Jupiter. Now, unexpectedly, a second such body had been found. When Pallas was discovered, some estimates of its size were as high as 3,380 km in diameter. Even as recently as 1979, Pallas was estimated to be 673 km in diameter (26% greater than the currently accepted value).
In 1917, the Japanese astronomer Kiyotsugu Hirayama began to study asteroid motions. By plotting the mean orbital motion, inclination and eccentricity of a set of asteroids, he discovered several distinct groupings. In a later paper he reported a group of three asteroids associated with Pallas, which became named the Pallas family after the largest member of the group. Since 1994 more than 10 members of this family have been identified, and these have semi-major axes between 2.50–2.82 AU and inclinations of 33–38°. The validity of this grouping was confirmed in 2002 by a comparison of their spectra.
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 resulted in the first accurate measurements of its diameter. During the occultation of May 29, 1979 the discovery of a possible tiny satellite with a diameter of about 1 km was reported. It could not be 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.
The Dawn Mission team was granted viewing time on the Hubble Space Telescope in September 2007 for a once-in-twenty-year opportunity to view the asteroid at closest approach, to obtain comparative data for Ceres and Vesta.
Both Vesta and Pallas have assumed the title of second-largest asteroid from time to time. However, Pallas is slightly larger than 4 Vesta in volume, but significantly less massive. The mass of Pallas is only 22% of Ceres and about 0.3% that of the Moon.
Pallas is farther from Earth and has a much lower albedo than Vesta, and so it appears dimmer. Indeed, the much smaller 7 Iris marginally exceeds Pallas in mean opposition magnitude. Pallas's mean opposition magnitude is +8.0, which is well within the range of 10×50 binoculars, but, unlike Ceres and Vesta, it will require more powerful optical aid to view at small elongations, when its magnitude can drop as low as +10.6. During rare perihelic oppositions, Pallas can reach a magnitude of +6.4, right on the edge of naked-eye visibility. During late February 2014 Pallas shone with magnitude 6.96.
Pallas has unusual dynamic parameters for such a large body. Its orbit is highly inclined and somewhat eccentric, despite being at the same distance from the Sun as the central part of the asteroid belt. Furthermore, its axial tilt is very high, either 78±13° or 65±12° (based on ambiguous lightcurve data, the pole points towards either ecliptic coordinates (β, λ) = (−12°, 35°) or (43°, 193°) with a 10° uncertainty; data from the Hubble Space Telescope obtained in 2007, as well as the observations by the Keck telescope in 2003–2005, favour the first solution.). This means that, every Palladian summer and winter, large parts of the surface are in constant sunlight or constant darkness for a time on the order of an Earth year.
Based on spectroscopic observations, the primary component of the Palladian surface material is a silicate that is low in iron and water. Minerals of this type include olivine and pyroxene, which are found in CM chondrules. The surface composition of Pallas is very similar to the Renazzo carbonaceous chondrite (CR) meteorites, which are even lower in hydrous minerals than the CM type. The Renazzo meteorite was discovered in Italy in 1824 and is one of the most primitive meteorites known.
Very little is known of Palladian surface features. Hubble images from 2007 show pixel-to-pixel variation (pixel resolution is around 70 kilometres (43 mi)), but Pallas's albedo of 0.12 placed such features at the lower end of detectability. There is little variability between lightcurves obtained through visible-light and infrared filters, but there are significant deviations in the ultraviolet, suggesting large surface or compositional features near 285° (75° west longitude). Pallas's rotation appears to be prograde.
Pallas is believed to have undergone at least some degree of thermal alteration and partial differentiation, which suggests that it is a remnant protoplanet. During the planetary formation stage of the Solar System, objects grew in size through an accretion process to approximately this size. Many of these objects were incorporated into larger bodies, which became the planets, whereas others were destroyed in collisions with other protoplanets. Pallas and Vesta are likely survivors from this early stage of planetary formation.
Pallas was among the "candidate planets" in an early draft of the IAU's 2006 definition of planet, but it does not qualify in the final definition because it has not "cleared the neighborhood" around its orbit. In the future, it is possible that Pallas may be classified as a dwarf planet, if it is found to have a surface that is in hydrostatic equilibrium.
Pallas is in a, likely coincidental, near-1:1 orbital resonance with Ceres. Pallas also has a near-18:7 resonance (91,000-year period) and an approximate 5:2 resonance (83-year period) with Jupiter.
Transits of planets from Pallas
From Pallas, Mercury, Venus, Mars, and Earth can occasionally appear to transit, or pass in front of, the Sun. Earth last did so in 1968 and 1998, and will next transit in 2224. Mercury did in October 2009. The last and next by Venus are in 1677 and 2123, and for Mars they are in 1597 and 2759.
It has been suggested that Pallas has a moon orbiting it on occasion, a moon about 1 kilometer in diameter was suggested based on occultation data from an occultation on May 29, 1978, and another one separated from Pallas by 750 kilometers and 175 kilometers in diameter itself was suggested in 1980, but later shown incorrect in 1983 occultation observations.
Theoretically it is relatively likely for Pallas to have a moon system, because it is by far the largest member of the Pallas family, and it is possible, considering that the other members are extremely small in comparison to Pallas, that some of the larger would-be members were caught into orbit of Pallas. However, considering the level at which it has been studied and observed since it was discovered, it is unlikely there are any large moons orbiting Pallas.
- Pallasite meteorites are not named for the asteroid, but for a scientist who characterized them. They do not necessarily share their origin with Pallas.
- A member of the Dawn team explained, "It is impossible to reach with a mission in the same class as Dawn because it takes too much thrust to reach Pallas. Pallas is highly inclined to the ecliptic plane. A lot of energy is needed to climb out of the ecliptic plane especially as far out of the plane as Pallas is. I did try to design a mission to reach Pallas and it was impossible with the Dawn spacecraft even if we went nowhere else than Pallas."
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- Unicode value U+26B4
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|Look up Pallas in Wiktionary, the free dictionary.|
|Wikimedia Commons has media related to (2) Pallas.|
- Mona Gable. "Study of first high-resolution images of Pallas confirms asteroid is actually a protoplanet". University of California, Los Angeles (UCLA). Archived from the original on 15 October 2009. Retrieved October 20, 2009.
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