VLT image of Pallas
|Discovered by||Heinrich Wilhelm Olbers|
|Discovery date||28 March 1802|
|MPC designation||(2) Pallas|
|asteroid belt · (central)|
|Adjectives||Palladian // |
|Orbital characteristics |
|Epoch 23 March 2018 (JD 2458200.5)|
|Uncertainty parameter 0|
|Observation arc||196.71 yr (71,847 d)|
|Earliest precovery date||1779|
|4.62 yr (1,686 d)|
|0° 12m 48.6s / day|
(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||km × 516 km × 476 km550 |
Equatorial surface gravity
|≈ 0.21 m/s² (average)[d]|
Equatorial escape velocity
|≈ 0.33 km/s[d]|
Equatorial rotation velocity
|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 is one of the largest asteroids in the Solar System. With an estimated 7% of the mass of the asteroid belt, it is the third-most-massive asteroid, being 10–30% less massive than Vesta. It is 512 kilometers (318 mi) in diameter, somewhat smaller than 4 Vesta. It is likely a remnant protoplanet.
When Pallas was discovered by the German astronomer Heinrich Wilhelm Matthäus Olbers on 28 March 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.
Pallas's surface is most likely composed of a silicate material; its spectrum and estimated density resemble carbonaceous chondrite meteorites. With an orbital inclination of 34.8°, Pallas's orbit is unusually highly inclined to the plane of the asteroid belt, and its orbital eccentricity is nearly as large as that of Pluto, making Pallas relatively inaccessible to spacecraft.[e]
It was considered as a potential planet in 2006, but it has since been determined that its shape departs significantly from an ellipsoid.
On the night of April 5, 1779, Charles Messier recorded Pallas on a star chart he used to track the path of a comet (now known as C/1779 A1 (Bode)) that he observed in the spring of 1779, but apparently assumed it was nothing more than a star.
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 that year by the Baron von Zach and Heinrich W. M. Olbers after a preliminary orbit was computed by Carl 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 stars several times, including the best observed of all asteroid occultation events on 29 May 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 29 May 1979 the discovery of a possible tiny satellite with a diameter of about 1 km was reported, which was never confirmed. In 1980, speckle interferometry was reported as indicating a much larger satellite with a diameter of 175 km, whose existence was later refuted.
The Dawn team was granted viewing time on the Hubble Space Telescope in September 2007 for a once-in-twenty-year opportunity to view Pallas at closest approach, to obtain comparative data for Ceres and Vesta.
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.
Orbit and rotation
Pallas has unusual dynamic parameters for such a large body. Its orbit is highly inclined and moderately eccentric, despite being at the same distance from the Sun as the central part of the asteroid belt. Furthermore, Pallas has a very high axial tilt of 84°, with its north pole pointing towards ecliptic coordinates (β, λ) = (30°, −16°) with a 5° uncertainty in the Ecliptic J2000.0 reference frame. 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, with areas near the poles experiencing continuous sunlight for as long as two years.
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.
An animation of Pallas's near-18:7 resonance with Jupiter. The orbit of Pallas is green when above the ecliptic and red when below. It only marches clockwise: it never halts or reverses course (i.e. no libration). The motion of Pallas is shown in a reference frame that rotates about the Sun (the center dot) with a period equal to Jupiter's orbital period. Accordingly, Jupiter's orbit appears almost stationary as the pink ellipse at top left. Mars's motion is orange, and the Earth–Moon system is blue and white.
Transits of planets from Pallas
From Pallas, the planets 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.
Both Vesta and Pallas have assumed the title of second-largest asteroid from time to time. At ±3 km in diameter, 512 Pallas is slightly smaller than Vesta (±0.2 km525.4). The mass of Pallas is only 84%+7%
−13% that of Vesta, 22% that of Ceres and about 0.3% that of the Moon.
Pallas is farther from Earth and has a much lower albedo than Vesta, and hence is dimmer as seen from Earth. 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.
Based on spectroscopic observations, the primary component of the material on Pallas's surface is a silicate containing little 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. Pallas's visible and near-infrared spectrum is almost flat, being slightly brighter in towards the blue. There is only one clear absorption band in the 3-micron part, which suggests an anhydrous component mixed with hydrated CM-like silicates.
Very little is known of Pallas's surface features. Hubble images from 2007, with a resolution around 70 kilometres (43 mi) per pixel, show pixel-to-pixel variation, 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 thought 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.
It has been suggested that Pallas has a moon. A moon about 1 kilometer in diameter was suggested based on occultation data from an occultation on 29 May 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. Considering the level at which Pallas has been studied and observed since it was discovered, it is unlikely that there are any large moons orbiting Pallas.
Pallas has not been visited by spacecraft. A flyby after the Dawn probe's visits to 4 Vesta and 1 Ceres was discussed but was not possible. The proposed Athena SmallSat mission, if funded, would be launched in 2022 as a secondary payload of the Psyche mission and would travel on separate trajectory to a flyby encounter with 2 Pallas.
- Calculated using the known dimensions assuming an ellipsoid.
- 1.06 ± 0.13 × 10−10 M☉
- Calculated by dividing the listed mass by the listed volume
- Calculated using the mean radius
- Pallasite meteorites are not named after the asteroid, but after the scientist who characterized them. They do not necessarily share their origin with Pallas.
- Unicode value U+26B4
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|Look up Pallas in Wiktionary, the free dictionary.|
|Wikimedia Commons has media related to (2) Pallas.|
- Pallas at Encyclopædia Britannica, Edward F. Tedesco
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