2 Pallas


Pallas (minor-planet designation: 2 Pallas) is the second asteroid to have been discovered, after Ceres. It is believed to have a mineral composition similar to carbonaceous chondrite meteorites, like Ceres, though significantly less hydrated than Ceres. It is the third-largest asteroid in the Solar System by both volume and mass, and is a likely remnant protoplanet. It is 79% the mass of Vesta and 22% the mass of Ceres, constituting an estimated 7% of the mass of the asteroid belt. Its estimated volume is equivalent to a sphere 507 to 515 kilometers (315 to 320 mi) in diameter, 90–95% the volume of Vesta.

2 Pallas
VLT-SPHERE image of Pallas[1]
Discovered byHeinrich Wilhelm Olbers
Discovery date28 March 1802
(2) Pallas
Named after
Pallas Athena[4]
Asteroid belt (central)
Pallas family[5]
AdjectivesPalladian (/pæˈldiən/)[6]
Symbol⚴ (historically astronomical, now astrological)
Orbital characteristics[7]
Epoch 13 September 2023
(JD 2453300.5)
Uncertainty parameter 0
Observation arc219 yr
Aphelion3.41 AU (510 million km)
Perihelion2.13 AU (319 million km)
2.77 AU (414 million km)
4.611 yr (1,684.0 d)
0° 12m 46.8s / day
(34.43° to invariable plane)[8]
7 March 2023
Earth MOID1.2 AU (180 million km)
Proper orbital elements[9]
2.7709176 AU
78.041654 deg / yr
4.61292 yr
(1684.869 d)
Precession of perihelion
−1.335344 arcsec / yr
Precession of the ascending node
−46.393342 arcsec / yr
Physical characteristics
Dimensionsc/a = 0.79±0.03[10]
568 ±12 km × 532 ±12 km × 448 ±12 km[11]
550 km × 516 km × 476 km[12]
Mean diameter
513±6 km[11]
512±6 km[12]
(8.3±0.2)×105 km2 (2020)[a][13]
Volume(7.06±0.3)×107 km3 (2020)[11]
Mass(2.04±0.03)×1020 kg average est.[11]
(2.01±0.13)×1020 kg[b][14]
Mean density
2.92±0.08 g/cm3[10]
2.89±0.08 g/cm3[11]
2.57±0.19 g/cm3[14]
Equatorial surface gravity
≈0.21 m/s2 (average)[c]
0.022 g
Equatorial escape velocity
324 m/s[11]
7.8132 h[15]
Equatorial rotation velocity
65 m/s[a]
6.49[18] to 10.65
0.629″ to 0.171″[19]

During the planetary formation era of the Solar System, objects grew in size through an accretion process to approximately the size of Pallas. Most of these protoplanets were incorporated into the growth of larger bodies, which became the planets, whereas others were ejected by the planets or destroyed in collisions with each other. Pallas, Vesta and Ceres appear to be the only intact bodies from this early stage of planetary formation to survive within the orbit of Neptune.[20]

When Pallas was discovered by the German astronomer Heinrich Wilhelm Matthäus Olbers on 28 March 1802, it was considered to be a planet,[21] as were other asteroids in the early 19th century. The discovery of many more asteroids after 1845 eventually led to the separate listing of "minor" planets from "major" planets, and the realization in the 1950s that such small bodies did not form in the same way as (other) planets led to the gradual abandonment of the term "minor planet" in favor of "asteroid" (or, for larger bodies such as Pallas, "planetoid").

With an orbital inclination of 34.8°, Pallas's orbit is unusually highly inclined to the plane of the asteroid belt, making Pallas relatively inaccessible to spacecraft, and its orbital eccentricity is nearly as large as that of Pluto.[22]

The high inclination of the orbit of Pallas results in the possibility of close conjunctions to stars that other solar objects always pass at great angular distance. This resulted in Pallas passing Sirius on 9 October 2022, only 8.5 arcminutes southwards,[23] while no planet can get closer than 30 degrees to Sirius.

History edit

Size comparison: the first 10 asteroids profiled against the Moon. Pallas is number two.

Discovery edit

On the night of 5 April 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.[24]

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.[25][26]

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.[27] When Pallas was discovered, some estimates of its size were as high as 3,380 km in diameter.[28] Even as recently as 1979, Pallas was estimated to be 673 km in diameter, 26% greater than the currently accepted value.[29]

The orbit of Pallas was determined by Gauss, who found the period of 4.6 years was similar to the period for Ceres. Pallas has a relatively high orbital inclination to the plane of the ecliptic.[27]

Later observations edit

High-resolution images of the north (at left) and south (at right) hemispheres of Pallas, made possible by the Adaptive-Optics (AO)-fed SPHERE imager on the Very Large Telescope (VLT) in 2020.[30] Two large impact basins could have been created by asteroid family–forming impacts. The bright spot in the southern hemisphere is reminiscent of the salt deposits on Ceres.

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.[31] Since 1994 more than 10 members of this family have been identified, with semi-major axes between 2.50 and 2.82 AU and inclinations of 33–38°.[32] The validity of the family was confirmed in 2002 by a comparison of their spectra.[33]

Pallas has been observed occulting stars several times, including the best-observed of all asteroid occultation events, by 140 observers on 29 May 1983. These measurements resulted in the first accurate calculation of its diameter.[34][35] After an occultation on 29 May 1979, the discovery of a possible tiny satellite with a diameter of about 1 km was reported, which was never confirmed.

Radio 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.[36]

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.[37][38]

Name and symbol edit

Pallas is an epithet of the Greek goddess Athena (Ancient Greek: Παλλάς Ἀθηνᾶ).[39][40] In some versions of the myth, Athena killed Pallas, daughter of Triton, then adopted her friend's name out of mourning.[41]

The adjectival form of the name is Palladian.[6] The d is part of the oblique stem of the Greek name, which appears before a vowel but disappears before the nominative ending -s. The oblique form is seen in the Italian and Russian names for the asteroid, Pallade and Паллада (Pallada).[42] The stony-iron pallasite meteorites are not Palladian, being named instead 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.[43]

The symbols for Ceres and Pallas, as published in 1802

The old astronomical symbol of Pallas, still used in astrology, is a spear or lance,  , one of the symbols of the goddess. The blade was most often a lozenge (), but various graphic variants were published, including an acute/elliptic leaf shape, a cordate leaf shape (:  ), and a triangle (); the last made it effectively the alchemical symbol for sulfur,  . The generic asteroid symbol of a disk with its discovery number, ⟨②⟩, was introduced in 1852 and quickly became the norm.[44][45] The iconic lozenge symbol was resurrected for astrological use in 1973.[46]

Orbit and rotation edit

Pallas has a high eccentricity and a highly inclined orbit

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.[12] 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.[12]

Near resonances edit

Pallas is in a near-1:1 orbital resonance with Ceres, which is probably coincidental.[47] Pallas also has a near-18:7 resonance (91,000-year period) and an approximate 5:2 resonance (83-year period) with Jupiter.[48]

Transits of planets from Pallas edit

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.[49]

Physical characteristics edit

Relative sizes of the four largest asteroids. Pallas is second from right.
The mass of 2 Pallas (blue) compared to other large asteroids: 4 Vesta, 10 Hygiea, 704 Interamnia, 15 Eunomia, the remainder of the Main Belt, and 1 Ceres. The unit of mass is ×1018 kg.

Both Vesta and Pallas have assumed the title of second-largest asteroid from time to time.[50] At 513±3 km in diameter,[11] Pallas is slightly smaller than Vesta (525.4±0.2 km[51]). The mass of Pallas is 79%±1% that of Vesta, 22% that of Ceres, and a quarter of one percent 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 asteroid 7 Iris marginally exceeds Pallas in mean opposition magnitude.[52] 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.[18] During late February 2014 Pallas shone with magnitude 6.96.[53]

Pallas is a B-type asteroid.[12] 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.[54] 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.[55] The Renazzo meteorite was discovered in Italy in 1824 and is one of the most primitive meteorites known.[56][d] 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.[12]

Pallas's surface is most likely composed of a silicate material; its spectrum and calculated density (2.89±0.08 g/cm3) correspond to CM chondrite meteorites (2.90±0.08 g/cm3), suggesting a mineral composition similar to that of Ceres, but significantly less hydrated.

To within observational limits, Pallas appears to be saturated with craters. Its high inclination and eccentricity means that average impacts are much more energetic than on Vesta or Ceres (with on average twice their velocity), meaning that smaller (and thus more common) impactors can create equivalently sized craters. Indeed, Pallas appears to have many more large craters than either Vesta or Ceres, with craters larger than 40 km covering at least 9% of its surface.[11]

Pallas's shape departs significantly from the dimensions of an equilibrium body at its current rotational period, indicating that it is not a dwarf planet.[12] It's possible that a suspected large impact basin at the south pole, which ejected 6%±1% of the volume of Pallas (twice the volume of the Rheasilvia basin on Vesta), may have increased its inclination and slowed its rotation; the shape of Pallas without such a basin would be close to an equilibrium shape for a 6.2-hour rotational period.[11] A smaller crater near the equator is associated with the Palladian family of asteroids.[11]

Pallas probably has a quite homogeneous interior. The close match between Pallas and CM chondrites suggests that they formed in the same era and that the interior of Pallas never reached the temperature (≈820 K) needed to dehydrate silicates, which would be necessary to differentiate a dry silicate core beneath a hydrated mantle. Thus Pallas should be rather homogeneous in composition, though some upward flow of water could have occurred since. Such a migration of water to the surface would have left salt deposits, potentially explaining Pallas's relatively high albedo. Indeed, one bright spot is reminiscent of those found on Ceres. Although other explanations for the bright spot are possible (e.g. a recent ejecta blanket), if the near-Earth asteroid 3200 Phaethon is an ejected piece of Pallas, as some have theorized, then a Palladian surface enriched in salts would explain the sodium abundance in the Geminid meteor shower caused by Phaethon.[11]

Surface features edit

Besides one bright spot in the southern hemisphere, the only surface features identified on Pallas are craters. As of 2020, 36 craters have been identified, 34 of which are larger than 40 km in diameter. Provisional names have been provided for some of them. The craters are named after ancient weapons.[11]

Features on Pallas (southern hemisphere)
Feature Pronunciation Latin or Greek Meaning
Akontia /əˈkɒntiə/ ἀκόντιον dart
Doru /ˈdr/ δόρυ pike
Hoplon /ˈhɒplɒn/ ὅπλον a weapon (esp. a large shield)
Kopis /ˈkpɪs/ κοπίς a large knife
Sarissa /səˈrɪsə/ σάρισσα lance
Sfendonai /ˈsfɛndən/ σφενδόνη slingstone
Toxa /ˈtɒksə/ τόξον bow
Xiphos /ˈzfɒs/ ξίΦος sword
Xyston /ˈzɪstɒn/ ξυστόν spear
Features on Pallas (northern hemisphere)
Feature Pronunciation Latin or Greek Meaning
Aklys /ˈklɪs/ āclys a small javelin attached to a strap
Falcata /fælˈktə/ falcāta a sword of pre-Roman Iberia
Makhaira /məˈkrə/ μάχαιρα a sword of ancient Greece
Pilum /ˈpləm/ pīlum a Roman javelin
Scutum /ˈskjuːtəm/ scūtum a Roman leather-covered shield
Sica /ˈskə/ sīca a dagger
Spatha /ˈspθə/ spatha a straight sword

Satellites edit

A small moon about 1 kilometer in diameter was suggested based on occultation data from 29 May 1978. In 1980, speckle interferometry suggested a much larger satellite, whose existence was later refuted a few years later with occultation data.[57]

Exploration edit

Pallas itself has never been visited by spacecraft. Proposals have been made in the past though none have come to fruition. A flyby of the Dawn probe's visits to 4 Vesta and 1 Ceres was discussed but was not possible due to the high orbital inclination of Pallas.[58][59] The proposed Athena SmallSat mission would have been launched in 2022 as a secondary payload of the Psyche mission and travel on separate trajectory to a flyby encounter with 2 Pallas,[60][61] though was not funded due to being outcompeted by other mission concepts such as the Transorbital Trailblazer Lunar Orbiter. The authors of the proposal cited Pallas as the "largest unexplored" protoplanet with the main belt.[62][63]

Gallery edit

See also edit

Notes edit

  1. ^ a b Calculated using the known dimensions assuming an ellipsoid.
  2. ^ (1.010 ± 0.065) × 10−10 M
  3. ^ Calculated using the mean radius
  4. ^ Marsset 2020 finds it closer to CM meteorites

References edit

  1. ^ The craters covering Pallas, here only faintly discernible, are likely to look much sharper if the view were closer, as can be seen in this comparison of VLT and Dawn images of 4 Vesta.
  2. ^ "2 Pallas". Minor Planet Center. Retrieved 1 June 2018.
  3. ^ "Pallas". Dictionary.com Unabridged (Online). n.d.
  4. ^ Schmadel, Lutz D. (2007). "(2) Pallas". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 15. doi:10.1007/978-3-540-29925-7_3. ISBN 978-3-540-00238-3.
  5. ^ "Asteroid 2 Pallas". Small Bodies Data Ferret. Retrieved 24 October 2019.
  6. ^ a b "Palladian". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
  7. ^ a b "JPL Small-Body Database Browser: 2 Pallas" (2018-01-23 last obs.). Jet Propulsion Laboratory. Retrieved 1 June 2018.
  8. ^ Souami, D.; Souchay, J. (July 2012). "The solar system's invariable plane". Astronomy & Astrophysics. 543: 11. Bibcode:2012A&A...543A.133S. doi:10.1051/0004-6361/201219011. A133.
  9. ^ "AstDyS-2 Pallas Synthetic Proper Orbital Elements". Department of Mathematics, University of Pisa, Italy. Retrieved 1 October 2011.
  10. ^ a b c d P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. Astronomy & Astrophysics 54, A56
  11. ^ a b c d e f g h i j k l Marsset, M, Brož, M, Vernazza, P, et al. (2020). "The violent collisional history of aqueously evolved (2) Pallas" (PDF). Nature Astronomy. 4 (6): 569–576. Bibcode:2020NatAs...4..569M. doi:10.1038/s41550-019-1007-5. hdl:10261/237549. S2CID 212927521.
  12. ^ a b c d e f g h Carry, B.; et al. (2009). "Physical properties of (2) Pallas". Icarus. 205 (2): 460–472. arXiv:0912.3626. Bibcode:2010Icar..205..460C. doi:10.1016/j.icarus.2009.08.007. S2CID 119194526.
  13. ^ "Surface-area calculation using Wolfram Alpha".
  14. ^ a b Baer, James; Chesley, Steven; Matson, Robert (2011). "Astrometric masses of 26 asteroids and observations on asteroid porosity". The Astronomical Journal. 141 (5): 143. Bibcode:2011AJ....141..143B. doi:10.1088/0004-6256/141/5/143.
  15. ^ "LCDB Data for (2) Pallas". Asteroid Lightcurve Database (LCDB). Retrieved 1 June 2018.
  16. ^ a b Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T. Retrieved 30 October 2019.
  17. ^ Neese, C., ed. (2005). "Asteroid Taxonomy. EAR-A-5-DDR-Taxonomy-V5.0". NASA Planetary Data System. Archived from the original on 5 August 2009. Retrieved 15 March 2007.
  18. ^ a b Menzel, Donald H.; Pasachoff, Jay M. (1983). A Field Guide to the Stars and Planets (2nd ed.). Boston, MA: Houghton Mifflin. p. 391. ISBN 978-0-395-34835-2.
  19. ^ Calculated with JPL Horizons for 1608-Feb-15
  20. ^ McCord, T. B.; McFadden, L. A.; Russell, C. T.; Sotin, C.; Thomas, P. C. (2006). "Ceres, Vesta, and Pallas: Protoplanets, Not Asteroids". Transactions of the American Geophysical Union. 87 (10): 105. Bibcode:2006EOSTr..87..105M. doi:10.1029/2006EO100002.
  21. ^ Hilton, James L. "When did the asteroids become minor planets?". Astronomical Applications Department. US Naval Observatory. Archived from the original on 6 April 2019. Retrieved 27 March 2019.
  22. ^ Anonymous. "Space Topics: Asteroids and Comets, Notable Comets". The Planetary Society. Archived from the original on 16 May 2008. Retrieved 28 June 2008.
  23. ^ Astrolutz 2022, ISBN 978-3-7534-7124-2
  24. ^ René Bourtembourg (2012). "Messier's Missed Discovery of Pallas in April 1779". Journal for the History of Astronomy. 43 (2): 209–214. Bibcode:2012JHA....43..209B. doi:10.1177/002182861204300205. S2CID 118405076.
  25. ^ Hoskin, Michael (26 June 1992). "Bode's Law and the Discovery of Ceres". Observatorio Astronomico di Palermo "Giuseppe S. Vaiana". Retrieved 5 July 2007.
  26. ^ Forbes, Eric G. (1971). "Gauss and the Discovery of Ceres". Journal for the History of Astronomy. 2 (3): 195–199. Bibcode:1971JHA.....2..195F. doi:10.1177/002182867100200305. S2CID 125888612.
  27. ^ a b "Astronomical Serendipity". NASA JPL. Archived from the original on 6 February 2012. Retrieved 15 March 2007.
  28. ^ Hilton, James L. (16 November 2007). "When did asteroids become minor planets?". U.S. Naval Observatory. Archived from the original on 21 September 2007. Retrieved 5 February 2014.
  29. ^ Hilton, James L. "Asteroid Masses and Densities" (PDF). U.S. Naval Observatory. Archived (PDF) from the original on 19 August 2008. Retrieved 7 September 2008.
  30. ^ "Golf Ball World". Retrieved 24 February 2020.
  31. ^ Kozai, Yoshihide (29 November – 3 December 1993). "Kiyotsugu Hirayama and His Families of Asteroids (invited)". Proceedings of the International Conference. Sagamihara, Japan: Astronomical Society of the Pacific. Bibcode:1994ASPC...63....1K.
  32. ^ Faure, Gérard (20 May 2004). "Description of the System of Asteroids". Astrosurf.com. Archived from the original on 2 February 2007. Retrieved 15 March 2007.
  33. ^ Foglia, S.; Masi, G. (1999). "New clusters for highly inclined main-belt asteroids". The Minor Planet Bulletin. 31 (4): 100–102. Bibcode:2004MPBu...31..100F. Archived from the original on 19 July 2011. Retrieved 15 March 2007.
  34. ^ Drummond, J. D.; Cocke, W. J. (1989). "Triaxial ellipsoid dimensions and rotational pole of 2 Pallas from two stellar occultations" (PDF). Icarus. 78 (2): 323–329. Bibcode:1989Icar...78..323D. CiteSeerX doi:10.1016/0019-1035(89)90180-2. Archived (PDF) from the original on 13 May 2011.
  35. ^ Dunham, D. W.; et al. (1990). "The size and shape of (2) Pallas from the 1983 occultation of 1 Vulpeculae". Astronomical Journal. 99: 1636–1662. Bibcode:1990AJ.....99.1636D. doi:10.1086/115446.
  36. ^ Pitjeva, E. V. (2004). "Estimations of masses of the largest asteroids and the main asteroid belt from ranging to planets, Mars orbiters and landers". 35th COSPAR Scientific Assembly. Held 18–25 July 2004, in Paris, France. p. 2014. Bibcode:2004cosp...35.2014P.
  37. ^ Schmidt, B.E.; Thomas, P.C.; Bauer, J.M.; Li, J.-Y.; McFadden, L.A.; Parker, J.M.; Rivkin, A.S.; Russell, C.T.; Stern, S.A. (2008). "Hubble takes a look at Pallas: Shape, size, and surface" (PDF). 39th Lunar and Planetary Science Conference (Lunar and Planetary Science XXXIX). Held 10–14 March 2008, in League City, Texas. 1391 (1391): 2502. Bibcode:2008LPI....39.2502S. Archived (PDF) from the original on 4 October 2008. Retrieved 24 August 2008.
  38. ^ Staff (24 October 2007). "Hubble Images of Asteroids Help Astronomers Prepare for Spacecraft Visit". JPL/NASA. Archived from the original on 9 June 2007. Retrieved 27 October 2007.
  39. ^ James, Andrew (1 September 2006). "Pallas". Southern Astronomical Delights. Retrieved 29 March 2007.
  40. ^ Freese, John Henry (1911). "Athena" . In Chisholm, Hugh (ed.). Encyclopædia Britannica. Vol. 2 (11th ed.). Cambridge University Press. p. 828.
  41. ^ Dietrich, Thomas (2005). The Origin of Culture and Civilization: The Cosmological Philosophy of the Ancient Worldview Regarding Myth, Astrology, Science, and Religion. Turnkey Press. p. 178. ISBN 978-0-9764981-6-2.
  42. ^ The one exception internationally to the use of the Greek stem for the name of the asteroid is Chinese, in which it is known as 智神星 (Zhìshénxīng), the 'wisdom-god star'.
  43. ^ "Palladium". Los Alamos National Laboratory. Archived from the original on 5 April 2007. Retrieved 28 March 2007.
  44. ^ Forbes, Eric G. (1971). "Gauss and the Discovery of Ceres". Journal for the History of Astronomy. 2 (3): 195–199. Bibcode:1971JHA.....2..195F. doi:10.1177/002182867100200305. S2CID 125888612. Archived from the original on 18 July 2021. Retrieved 18 July 2021.
  45. ^ Gould, B. A. (1852). "On the symbolic notation of the asteroids". Astronomical Journal. 2 (34): 80. Bibcode:1852AJ......2...80G. doi:10.1086/100212.
  46. ^ Eleanor Bach (1973) Ephemerides of the asteroids: Ceres, Pallas, Juno, Vesta, 1900–2000. Celestial Communications.
  47. ^ Goffin, E. (2001). "New determination of the mass of Pallas". Astronomy and Astrophysics. 365 (3): 627–630. Bibcode:2001A&A...365..627G. doi:10.1051/0004-6361:20000023.
  48. ^ Taylor, D. B. (1982). "The secular motion of Pallas". Monthly Notices of the Royal Astronomical Society. 199 (2): 255–265. Bibcode:1982MNRAS.199..255T. doi:10.1093/mnras/199.2.255.
  49. ^ "Solex by Aldo Vitagliano". Archived from the original on 20 December 2008. Retrieved 19 March 2009. (numbers generated by Solex)
  50. ^ "Notable Asteroids". The Planetary Society. 2007. Archived from the original on 16 April 2007. Retrieved 17 March 2007.
  51. ^ Russell, C. T.; et al. (2012). "Dawn at Vesta: Testing the Protoplanetary Paradigm". Science. 336 (6082): 684–686. Bibcode:2012Sci...336..684R. doi:10.1126/science.1219381. PMID 22582253. S2CID 206540168.
  52. ^ Odeh, Moh'd. "The Brightest Asteroids". Jordanian Astronomical Society. Archived from the original on 13 August 2007. Retrieved 16 July 2007.
  53. ^ Calculated with JPL Horizons for 2014-Feb-24
  54. ^ Feierberg, M. A.; Larson, H. P.; Lebofsky, L. A. (1982). "The 3 Micron Spectrum of Asteroid 2 Pallas". Bulletin of the American Astronomical Society. 14: 719. Bibcode:1982BAAS...14..719F.
  55. ^ Sato, Kimiyasu; Miyamoto, Masamichi; Zolensky, Michael E. (1997). "Absorption bands near 3 m in diffuse reflectance spectra of carbonaceous chondrites: Comparison with asteroids". Meteoritics. 32 (4): 503–507. Bibcode:1997M&PS...32..503S. doi:10.1111/j.1945-5100.1997.tb01295.x. S2CID 129687767.
  56. ^ "Earliest Meteorites Provide New Piece in Planetary Formation Puzzle". Particle Physics and Astronomy Research Council. 20 September 2005. Archived from the original on 6 May 2013. Retrieved 24 May 2006.
  57. ^ Johnston, William Robert (5 March 2007). "Other Reports of Asteroid/TNO Companions". Johnson's Archive. Archived from the original on 10 February 2007. Retrieved 14 March 2007.
  58. ^ Rayman, Marc (29 December 2014). "Ceres' Curiosities: The Mysterious World Comes Into View". NASA Jet Propulsion Laboratory. Archived from the original on 17 February 2015. Retrieved 20 September 2021.
  59. ^ Perozzi, Ettore; Rossi, Alessandro; Valsecchi, Giovanni B. (2001). "Basic targeting strategies for rendezvous and flyby missions to the near-Earth asteroids". Planetary and Space Science. 49 (1): 3–22. Bibcode:2001P&SS...49....3P. doi:10.1016/S0032-0633(00)00124-0.
  60. ^ Dorminey, Bruce (10 March 2019). "Proposed NASA SmallSat Mission Could Be First To Visit Pallas, Our Third Largest Asteroid". Forbes. Retrieved 10 March 2019.
  61. ^ Athena: the first-ever encounter of (2) Pallas with a Smallsat. J. G. O'Rourke, J. Castillo-Rogez, L. T. Elkins-Tanton, R. R. Fu, T. N. Harrison, S. Marchi, R. Park, B. E. Schmidt, D. A. Williams, C. C. Seybold, R. N. Schindhelm, J. D. Weinberg. 50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132).
  62. ^ "Finalists Selected for NASA's SIMPLEx Program". Planetary News. 24 June 2019. Archived from the original on 23 November 2020. Retrieved 20 September 2021.
  63. ^ "Athena: A SmallSat Mission to (2) Pallas". Archived from the original on 21 November 2021. Retrieved 7 October 2020.
  64. ^ Gingerich, Owen (16 August 2006). "The Path to Defining Planets" (PDF). Harvard-Smithsonian Center for Astrophysics and IAU EC Planet Definition Committee chair. p. 4. Archived (PDF) from the original on 15 March 2015. Retrieved 13 March 2007.

External links edit

  • Pallas at Encyclopædia Britannica, Edward F. Tedesco
  • 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 20 October 2009.
  • Jonathan Amos (11 October 2009). "Pallas is 'Peter Pan' space rock". BBC. Archived from the original on 19 July 2010. Retrieved 19 August 2010.
  • "2 Pallas". JPL Small-Body Database Browser. Retrieved 29 March 2007.
  • Dunn, Tony (2006). "Ceres, Pallas Vesta and Hygeia". GravitySimulator.com. Archived from the original on 13 March 2007. Retrieved 15 March 2007.
  • Hilton, James L. (1 April 1999). "U.S. Naval Observatory Ephemerides of the Largest Asteroids". U.S. Naval Observatory. Archived from the original on 23 July 2011. Retrieved 14 March 2007.
  • Tedesco, Edward F.; Noah, Paul V.; Noah, Meg; Price, Stephan D. (2002). "The Supplemental IRAS Minor Planet Survey". The Astronomical Journal. 123 (2): 1056–1085. Bibcode:2002AJ....123.1056T. doi:10.1086/338320.
  • 2 Pallas at AstDyS-2, Asteroids—Dynamic Site
    • Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
  • 2 Pallas at the JPL Small-Body Database  
    • Close approach · Discovery · Ephemeris · Orbit diagram · Orbital elements · Physical parameters