Wikipedia

4 Vesta

This article is about the asteroid. For the Roman goddess, see Vesta (mythology). For other uses, see Vesta (disambiguation).

Vesta (minor-planet designation: 4 Vesta) is one of the largest objects in the asteroid belt, with a mean diameter of 525 kilometres (326 mi).[10] It was discovered by the German astronomer Heinrich Wilhelm Matthias Olbers on 29 March 1807[6] and is named after Vesta, the virgin goddess of home and hearth from Roman mythology.[19]

4 Vesta
True color image of Vesta taken by Dawn. The massive Rheasilvia Crater dominates Vesta's south pole.
Discovery
Discovered byHeinrich Wilhelm Olbers
Discovery date29 March 1807
Designations
(4) Vesta
Pronunciation/ˈvɛstə/[1]
Named after
Vesta
Main belt (Vesta family)
Adjectives
  • Vestan
  • Vestian[a]
Symbol⚶ (historically astronomical, now astrological)
Orbital characteristics[6]
Epoch 13 September 2023
(JD 2453300.5)
Aphelion2.57 AU (384 million km)
Perihelion2.15 AU (322 million km)
2.36 AU (353 million km)
Eccentricity0.0894
3.63 yr (1325.86 d)
19.34 km/s
169.4°
Inclination7.1422° to ecliptic
5.58° to invariable plane[7]
103.71°
26 December 2021[8]
151.66°
SatellitesNone
Earth MOID1.14 AU (171 million km)
Proper orbital elements[9]
2.36151 AU
0.098758
6.39234°
99.1888 deg / yr
3.62944 yr
(1325.654 d)
Precession of perihelion
36.8729 (2343 years) arcsec / yr
Precession of the ascending node
−39.5979 (2182 years) arcsec / yr
Physical characteristics
Dimensions572.6 km × 557.2 km × 446.4 km[10]
525.4±0.2 km[10]
Flattening0.2204
(8.66±0.2)×105 km2[b][11]
Volume7.4970×107 km3[10]
Mass(2.590271±0.000058)×1020 kg[12]
Mean density
3.456±0.035 g/cm3[10]
Equatorial surface gravity
0.25 m/s2 (0.025 g0)
Equatorial escape velocity
0.36 km/s
0.2226 d (5.342 h)[6][13]
Equatorial rotation velocity
93.1 m/s[c]
29°
North pole right ascension
20h 32m[d]
North pole declination
48°[d]
0.423[15]
Temperaturemin: 75 K (−198 °C)
max: 250 K (−23 °C)[16]
V[6][17]
5.1[18] to 8.48
3.20[6][15]
0.70″ to 0.22″

Vesta is thought to be the second-largest asteroid, both by mass and by volume, after the dwarf planet Ceres.[20][21][22] Measurements give it a nominal volume only slightly larger than that of Pallas (about 5% greater), but it is 25% to 30% more massive. It constitutes an estimated 9% of the mass of the asteroid belt.[23] Vesta is the only known remaining rocky protoplanet (with a differentiated interior) of the kind that formed the terrestrial planets.[24][25][26] Numerous fragments of Vesta were ejected by collisions one and two billion years ago that left two enormous craters occupying much of Vesta's southern hemisphere.[27][28] Debris from these events has fallen to Earth as howardite–eucrite–diogenite (HED) meteorites, which have been a rich source of information about Vesta.[29][30][31]

Vesta is the brightest asteroid visible from Earth. It is regularly as bright as magnitude 5.1,[18] at which times it is faintly visible to the naked eye. Its maximum distance from the Sun is slightly greater than the minimum distance of Ceres from the Sun,[e] although its orbit lies entirely within that of Ceres.[32]

NASA's Dawn spacecraft entered orbit around Vesta on 16 July 2011 for a one-year exploration and left the orbit of Vesta on 5 September 2012[33] en route to its final destination, Ceres. Researchers continue to examine data collected by Dawn for additional insights into the formation and history of Vesta.[34][35]

History

edit

Discovery

edit
 
Vesta, Ceres, and the Moon with sizes shown to scale

Heinrich Olbers discovered Pallas in 1802, the year after the discovery of Ceres. He proposed that the two objects were the remnants of a destroyed planet. He sent a letter with his proposal to the British astronomer William Herschel, suggesting that a search near the locations where the orbits of Ceres and Pallas intersected might reveal more fragments. These orbital intersections were located in the constellations of Cetus and Virgo.[36] Olbers commenced his search in 1802, and on 29 March 1807 he discovered Vesta in the constellation Virgo—a coincidence, because Ceres, Pallas, and Vesta are not fragments of a larger body. Because the asteroid Juno had been discovered in 1804, this made Vesta the fourth object to be identified in the region that is now known as the asteroid belt. The discovery was announced in a letter addressed to German astronomer Johann H. Schröter dated 31 March.[37] Because Olbers already had credit for discovering a planet (Pallas; at the time, the asteroids were considered to be planets), he gave the honor of naming his new discovery to German mathematician Carl Friedrich Gauss, whose orbital calculations had enabled astronomers to confirm the existence of Ceres, the first asteroid, and who had computed the orbit of the new planet in the remarkably short time of 10 hours.[38][39] Gauss decided on the Roman virgin goddess of home and hearth, Vesta.[40]

Name and symbol

edit

Vesta was the fourth asteroid to be discovered, hence the number 4 in its formal designation. The name Vesta, or national variants thereof, is in international use with two exceptions: Greece and China. In Greek, the name adopted was the Hellenic equivalent of Vesta, Hestia (4 Εστία); in English, that name is used for 46 Hestia (Greeks use the name "Hestia" for both, with the minor-planet numbers used for disambiguation). In Chinese, Vesta is called the 'hearth-god(dess) star', 灶神星 Zàoshénxīng, naming the asteroid for Vesta's role, similar to the Chinese names of Uranus, Neptune, and Pluto.[f]

Upon its discovery, Vesta was, like Ceres, Pallas, and Juno before it, classified as a planet and given a planetary symbol. The symbol represented the altar of Vesta with its sacred fire and was designed by Gauss.[41][42] In Gauss's conception, now obsolete, this was drawn  . His form is in the pipeline for Unicode 17.0 as U+1F777 🝷.[43][44][g] The asteroid symbols were gradually retired from astronomical use after 1852, but the symbols for the first four asteroids were resurrected for astrology in the 1970s. The abbreviated modern astrological variant of the Vesta symbol is   (U+26B6 ⚶).[43][h]

After the discovery of Vesta, no further objects were discovered for 38 years, and during this time the Solar System was thought to have eleven planets.[49] However, in 1845, new asteroids started being discovered at a rapid pace, and by 1851 there were fifteen, each with its own symbol, in addition to the eight major planets (Neptune had been discovered in 1846). It soon became clear that it would be impractical to continue inventing new planetary symbols indefinitely, and some of the existing ones proved difficult to draw quickly. That year, the problem was addressed by Benjamin Apthorp Gould, who suggested numbering asteroids in their order of discovery, and placing this number in a disk (circle) as the generic symbol of an asteroid. Thus, the fourth asteroid, Vesta, acquired the generic symbol ④. This was soon coupled with the name into an official number–name designation, ④ Vesta, as the number of minor planets increased. By 1858, the circle had been simplified to parentheses, (4) Vesta, which were easier to typeset. Other punctuation, such as 4) Vesta and 4, Vesta, was also briefly used, but had more or less completely died out by 1949.[50]

Early measurements

edit
 
SPHERE image is shown on the left, with a synthetic view derived from Dawn images shown on the right for comparison.[51]

Photometric observations of Vesta were made at the Harvard College Observatory in 1880–1882 and at the Observatoire de Toulouse in 1909. These and other observations allowed the rotation rate of Vesta to be determined by the 1950s. However, the early estimates of the rotation rate came into question because the light curve included variations in both shape and albedo.[52]

Early estimates of the diameter of Vesta ranged from 383 kilometres (238 mi) in 1825, to 444 km (276 mi). E.C. Pickering produced an estimated diameter of 513 ± 17 km (319 ± 11 mi) in 1879, which is close to the modern value for the mean diameter, but the subsequent estimates ranged from a low of 390 km (242 mi) up to a high of 602 km (374 mi) during the next century. The measured estimates were based on photometry. In 1989, speckle interferometry was used to measure a dimension that varied between 498 and 548 km (309 and 341 mi) during the rotational period.[53] In 1991, an occultation of the star SAO 93228 by Vesta was observed from multiple locations in the eastern United States and Canada. Based on observations from 14 different sites, the best fit to the data was an elliptical profile with dimensions of about 550 km × 462 km (342 mi × 287 mi).[54] Dawn confirmed this measurement.[i] These measurements will help determine the thermal history, size of the core, role of water in asteroid evolution and what meteorites found on Earth come from these bodies, with the ultimate goal of understanding the conditions and processes present at the solar system's earliest epoch and the role of water content and size in planetary evolution.[55]

Vesta became the first asteroid to have its mass determined. Every 18 years, the asteroid 197 Arete approaches within 0.04 AU of Vesta. In 1966, based upon observations of Vesta's gravitational perturbations of Arete, Hans G. Hertz estimated the mass of Vesta at (1.20±0.08)×10−10 M☉ (solar masses).[56] More refined estimates followed, and in 2001 the perturbations of 17 Thetis were used to calculate the mass of Vesta to be (1.31±0.02)×10−10 M☉.[57] Dawn determined it to be 1.3029×10−10 M☉.

Orbit

edit

Vesta orbits the Sun between Mars and Jupiter, within the asteroid belt, with a period of 3.6 Earth years,[6] specifically in the inner asteroid belt, interior to the Kirkwood gap at 2.50 AU. Its orbit is moderately inclined (i = 7.1°, compared to 7° for Mercury and 17° for Pluto) and moderately eccentric (e = 0.09, about the same as for Mars).[6]

True orbital resonances between asteroids are considered unlikely. Because of their small masses relative to their large separations, such relationships should be very rare.[58] Nevertheless, Vesta is able to capture other asteroids into temporary 1:1 resonant orbital relationships (for periods up to 2 million years or more) and about forty such objects have been identified.[59] Decameter-sized objects detected in the vicinity of Vesta by Dawn may be such quasi-satellites rather than proper satellites.[59]

Rotation

edit
 
Olbers Regio (dark area) defines the prime meridian in the IAU coordinate system. It is shown here in a Hubble shot of Vesta, because it is not visible in the more detailed Dawn images.
 
Claudia crater (indicated by the arrow at the bottom of the closeup image at right) defines the prime meridian in the Dawn/NASA coordinate system.

Vesta's rotation is relatively fast for an asteroid (5.342 h) and prograde, with the north pole pointing in the direction of right ascension 20 h 32 min, declination +48° (in the constellation Cygnus) with an uncertainty of about 10°. This gives an axial tilt of 29°.[60]

Coordinate systems

edit

Two longitudinal coordinate systems are used for Vesta, with prime meridians separated by 150°. The IAU established a coordinate system in 1997 based on Hubble photos, with the prime meridian running through the center of Olbers Regio, a dark feature 200 km across. When Dawn arrived at Vesta, mission scientists found that the location of the pole assumed by the IAU was off by 10°, so that the IAU coordinate system drifted across the surface of Vesta at 0.06° per year, and also that Olbers Regio was not discernible from up close, and so was not adequate to define the prime meridian with the precision they needed. They corrected the pole, but also established a new prime meridian 4° from the center of Claudia, a sharply defined crater 700 meters across, which they say results in a more logical set of mapping quadrangles.[61] All NASA publications, including images and maps of Vesta, use the Claudian meridian, which is unacceptable to the IAU. The IAU Working Group on Cartographic Coordinates and Rotational Elements recommended a coordinate system, correcting the pole but rotating the Claudian longitude by 150° to coincide with Olbers Regio.[62] It was accepted by the IAU, although it disrupts the maps prepared by the Dawn team, which had been positioned so they would not bisect any major surface features.[61][63]

Physical characteristics

edit
 
Relative sizes of the four largest asteroids. Vesta is second from left.
The mass of 4 Vesta (blue) compared to other large asteroids: 1 Ceres, 2 Pallas, 10 Hygiea, 704 Interamnia, 15 Eunomia and the remainder of the Main Belt. The unit of mass is ×1018 kg. Other objects in the Solar system with well-defined masses within a factor of 2 of Vesta's mass are Varda, Gǃkúnǁʼhòmdímà, and Salacia (245, 136, and 492 ×1018 kg. respectively). No moons are in this range: the closest, Tethys (Saturn III) and Enceladus (Saturn II), are over twice and less than half of Vesta's mass.

Vesta is the second most massive body in the asteroid belt, although it is only 28% as massive as Ceres, the most massive body.[64][23] Vesta is however the most massive body that formed in the asteroid belt, as Ceres is believed to have formed between Jupiter and Saturn. Vesta's density is lower than those of the four terrestrial planets but is higher than those of most asteroids, as well as all of the moons in the Solar System except Io. Vesta's surface area is about the same as the land area of Pakistan, Venezuela, Tanzania, or Nigeria; slightly under 900,000 square kilometres (350,000 sq mi; 90,000,000 ha; 220,000,000 acres). It has a differentiated interior.[24] Vesta is only slightly larger (525.4±0.2 km[10]) than 2 Pallas (512±3 km) in mean diameter,[65] but is about 25% more massive.

Vesta's shape is close to a gravitationally relaxed oblate spheroid,[60] but the large concavity and protrusion at the southern pole (see 'Surface features' below) combined with a mass less than 5×1020 kg precluded Vesta from automatically being considered a dwarf planet under International Astronomical Union (IAU) Resolution XXVI 5.[66] A 2012 analysis of Vesta's shape[67] and gravity field using data gathered by the Dawn spacecraft has shown that Vesta is currently not in hydrostatic equilibrium.[10][68]

Temperatures on the surface have been estimated to lie between about −20 °C (253 K) with the Sun overhead, dropping to about −190 °C (83.1 K) at the winter pole. Typical daytime and nighttime temperatures are −60 °C (213 K) and −130 °C (143 K), respectively. This estimate is for 6 May 1996, very close to perihelion, although details vary somewhat with the seasons.[16]

Surface features

edit
Further information: List of geological features on Vesta

Before the arrival of the Dawn spacecraft, some Vestan surface features had already been resolved using the Hubble Space Telescope and ground-based telescopes (e.g., the Keck Observatory).[69] The arrival of Dawn in July 2011 revealed the complex surface of Vesta in detail.[70]

 
Geologic map of Vesta (Mollweide projection).[71] The most ancient and heavily cratered regions are brown; areas modified by the Veneneia and Rheasilvia impacts are purple (the Saturnalia Fossae Formation, in the north)[72] and light cyan (the Divalia Fossae Formation, equatorial),[71] respectively; the Rheasilvia impact basin interior (in the south) is dark blue, and neighboring areas of Rheasilvia ejecta (including an area within Veneneia) are light purple-blue;[73][74] areas modified by more recent impacts or mass wasting are yellow/orange or green, respectively.

Rheasilvia and Veneneia

edit
Main articles: Rheasilvia and Veneneia
 
Northern (left) and southern (right) hemispheres. The "Snowman" craters are at the top of the left image; Rheasilvia and Veneneia (green and blue) dominate the right. Parallel troughs are seen in both. Colors of the two hemispheres are not to scale,[j] and the equatorial region is not shown.
 
South pole of Vesta, showing the extent of Rheasilvia crater.

The most prominent of these surface features are two enormous impact basins, the 500-kilometre (311 mi)-wide Rheasilvia, centered near the south pole; and the 400 km (249 mi) wide Veneneia. The Rheasilvia impact basin is younger and overlies the Veneneia.[75] The Dawn science team named the younger, more prominent crater Rheasilvia, after the mother of Romulus and Remus and a mythical vestal virgin.[76] Its width is 95% of the mean diameter of Vesta. The crater is about 19 km (12 mi) deep. A central peak rises 23 km (14 mi) above the lowest measured part of the crater floor and the highest measured part of the crater rim is 31 km (19 mi) above the crater floor low point. It is estimated that the impact responsible excavated about 1% of the volume of Vesta, and it is likely that the Vesta family and V-type asteroids are the products of this collision. If this is the case, then the fact that 10 km (6.2 mi) fragments have survived bombardment until the present indicates that the crater is at most only about 1 billion years old.[77] It would also be the site of origin of the HED meteorites. All the known V-type asteroids taken together account for only about 6% of the ejected volume, with the rest presumably either in small fragments, ejected by approaching the 3:1 Kirkwood gap, or perturbed away by the Yarkovsky effect or radiation pressure. Spectroscopic analyses of the Hubble images have shown that this crater has penetrated deep through several distinct layers of the crust, and possibly into the mantle, as indicated by spectral signatures of olivine.[60]

The large peak at the center of Rheasilvia is 20 to 25 km (12–16 mi) high and 180 km (112 mi) wide,[75] and is possibly a result of a planetary-scale impact.[78]

Other craters

edit
 
The crater Aelia
 
Feralia Planitia, an old, degraded impact basin or impact basin complex near Vesta's equator (green and blue). It is 270 km (168 mi) across and predates Rheasilvia (green at bottom)

Several old, degraded craters approach Rheasilvia and Veneneia in size, although none are quite so large. They include Feralia Planitia, shown at right, which is 270 km (168 mi) across.[79] More-recent, sharper craters range up to 158 km (98 mi) Varronilla and 196 km (122 mi) Postumia.[80]

Dust fills up some craters, creating so-called dust ponds. They are a phenomenon where pockets of Dust are seen in Celestial bodies without a significant atmosphere. These are smooth deposits of dust accumulated in depressions on the surface of the body (like craters), contrasting from the Rocky terrain around them.[81] On the surface of Vesta, we have identified both type 1 (formed from impact melt) and type 2 (electrostatically made) dust ponds within 0˚–30°N/S, that is, Equatorial region. 10 craters have been identified with such formations.[82]

"Snowman craters"

edit

The "snowman craters" are a group of three adjacent craters in Vesta's northern hemisphere. Their official names, from largest to smallest (west to east), are Marcia, Calpurnia, and Minucia. Marcia is the youngest and cross-cuts Calpurnia. Minucia is the oldest.[71]

 
"Snowman" craters by Dawn from 5,200 km (3,200 mi) in 2011
 
Detailed image of the "Snowman" craters

Troughs

edit

The majority of the equatorial region of Vesta is sculpted by a series of parallel troughs designated Divalia Fossae; its longest trough is 10–20 kilometres (6.2–12.4 mi) wide and 465 kilometres (289 mi) long. Despite the fact that Vesta is a one-seventh the size of the Moon, Divalia Fossae dwarfs the Grand Canyon. A second series, inclined to the equator, is found further north. This northern trough system is named Saturnalia Fossae, with its largest trough being roughly 40 km wide and over 370 km long. These troughs are thought to be large-scale graben resulting from the impacts that created Rheasilvia and Veneneia craters, respectively. They are some of the longest chasms in the Solar System, nearly as long as Ithaca Chasma on Tethys. The troughs may be graben that formed after another asteroid collided with Vesta, a process that can happen only in a body that, like Vesta, is differentiated.[83] Vesta's differentiation is one of the reasons why scientists consider it a protoplanet.[84] Alternatively, it is proposed that the troughs may be radial sculptures created by secondary cratering from Rheasilvia. [85]

 
A section of Divalia Fossae, with parallel troughs to the north and south
 
A computer-generated view of a portion of Divalia Fossae

Surface composition

edit

Compositional information from the visible and infrared spectrometer (VIR), gamma-ray and neutron detector (GRaND), and framing camera (FC), all indicate that the majority of the surface composition of Vesta is consistent with the composition of the howardite, eucrite, and diogenite meteorites.[86][87][88] The Rheasilvia region is richest in diogenite, consistent with the Rheasilvia-forming impact excavating material from deeper within Vesta. The presence of olivine within the Rheasilvia region would also be consistent with excavation of mantle material. However, olivine has only been detected in localized regions of the northern hemisphere, not within Rheasilvia.[34] The origin of this olivine is currently unclear. Though olivine was expected by astronomers to have originated from Vesta's mantle prior to the arrival of the Dawn orbiter, the lack of olivine within the Rheasilvia and Veneneia impact basins complicates this view. Both impact basins excavated Vestian material down to 60–100 km, far deeper than the expected thickness of ~30–40 km for Vesta's crust. Vesta's crust may be far thicker than expected or the violent impact events that created Rheasilvia and Veneneia may have mixed material enough to obscure olivine from observations. Alternatively, Dawn observations of olivine could instead be due to delivery by olivine-rich impactors, unrelated to Vesta's internal structure.[89]

Features associated with volatiles

edit

Pitted terrain has been observed in four craters on Vesta: Marcia, Cornelia, Numisia and Licinia.[90] The formation of the pitted terrain is proposed to be degassing of impact-heated volatile-bearing material. Along with the pitted terrain, curvilinear gullies are found in Marcia and Cornelia craters. The curvilinear gullies end in lobate deposits, which are sometimes covered by pitted terrain, and are proposed to form by the transient flow of liquid water after buried deposits of ice were melted by the heat of the impacts.[72] Hydrated materials have also been detected, many of which are associated with areas of dark material.[91] Consequently, dark material is thought to be largely composed of carbonaceous chondrite, which was deposited on the surface by impacts. Carbonaceous chondrites are comparatively rich in mineralogically bound OH.[88]

Geology

edit
 
Cut-away schematic of Vestan core, mantle, and crust
 
Eucrite meteorite

A large collection of potential samples from Vesta is accessible to scientists, in the form of over 1200 HED meteorites (Vestan achondrites), giving insight into Vesta's geologic history and structure. NASA Infrared Telescope Facility (NASA IRTF) studies of asteroid (237442) 1999 TA10 suggest that it originated from deeper within Vesta than the HED meteorites.[25]

Vesta is thought to consist of a metallic iron–nickel core 214–226 km in diameter,[10] an overlying rocky olivine mantle, with a surface crust. From the first appearance of calcium–aluminium-rich inclusions (the first solid matter in the Solar System, forming about 4.567 billion years ago), a likely time line is as follows:[92][93][94][95][96]

Timeline of the evolution of Vesta
2–3 million years Accretion completed
4–5 million years Complete or almost complete melting due to radioactive decay of 26Al, leading to separation of the metal core
6–7 million years Progressive crystallization of a convecting molten mantle. Convection stopped when about 80% of the material had crystallized
Extrusion of the remaining molten material to form the crust, either as basaltic lavas in progressive eruptions, or possibly forming a short-lived magma ocean.
The deeper layers of the crust crystallize to form plutonic rocks, whereas older basalts are metamorphosed due to the pressure of newer surface layers.
Slow cooling of the interior

Vesta is the only known intact asteroid that has been resurfaced in this manner. Because of this, some scientists refer to Vesta as a protoplanet.[97] However, the presence of iron meteorites and achondritic meteorite classes without identified parent bodies indicates that there once were other differentiated planetesimals with igneous histories, which have since been shattered by impacts.[citation needed]

Composition of the Vestan crust (by depth)[98]
A lithified regolith, the source of howardites and brecciated eucrites.
Basaltic lava flows, a source of non-cumulate eucrites.
Plutonic rocks consisting of pyroxene, pigeonite and plagioclase, the source of cumulate eucrites.
Plutonic rocks rich in orthopyroxene with large grain sizes, the source of diogenites.

On the basis of the sizes of V-type asteroids (thought to be pieces of Vesta's crust ejected during large impacts), and the depth of Rheasilvia crater (see below), the crust is thought to be roughly 10 kilometres (6 mi) thick.[99] Findings from the Dawn spacecraft have found evidence that the troughs that wrap around Vesta could be graben formed by impact-induced faulting (see Troughs section above), meaning that Vesta has more complex geology than other asteroids. Vesta's differentiated interior implies that it was in hydrostatic equilibrium and thus a dwarf planet in the past, but it is not today.[75] The impacts that created the Rheasilvia and Veneneia craters occurred when Vesta was no longer warm and plastic enough to return to an equilibrium shape, distorting its once rounded shape and prohibiting it from being classified as a dwarf planet today.[citation needed]

Regolith

edit

Vesta's surface is covered by regolith distinct from that found on the Moon or asteroids such as Itokawa. This is because space weathering acts differently. Vesta's surface shows no significant trace of nanophase iron because the impact speeds on Vesta are too low to make rock melting and vaporization an appreciable process. Instead, regolith evolution is dominated by brecciation and subsequent mixing of bright and dark components.[100] The dark component is probably due to the infall of carbonaceous material, whereas the bright component is the original Vesta basaltic soil.[101]

Fragments

edit

Some small Solar System bodies are suspected to be fragments of Vesta caused by impacts. The Vestian asteroids and HED meteorites are examples. The V-type asteroid 1929 Kollaa has been determined to have a composition akin to cumulate eucrite meteorites, indicating its origin deep within Vesta's crust.[30]

Vesta is currently one of only eight identified Solar System bodies of which we have physical samples, coming from a number of meteorites suspected to be Vestan fragments. It is estimated that 1 out of 16 meteorites originated from Vesta.[102] The other identified Solar System samples are from Earth itself, meteorites from Mars, meteorites from the Moon, and samples returned from the Moon, the comet Wild 2, and the asteroids 25143 Itokawa, 162173 Ryugu, and 101955 Bennu.[31][k]

Exploration

edit
 
Animation of Dawn's trajectory from 27 September 2007 to 5 October 2018
   Dawn  ·   Earth ·   Mars ·   4 Vesta  ·   1 Ceres
 
First image of asteroids (Ceres and Vesta) taken from Mars. The image was made by the Curiosity rover on 20 April 2014.
 
Animation of Dawn's trajectory around 4 Vesta from 15 July 2011 to 10 September 2012
   Dawn ·   4 Vesta

In 1981, a proposal for an asteroid mission was submitted to the European Space Agency (ESA). Named the Asteroidal Gravity Optical and Radar Analysis (AGORA), this spacecraft was to launch some time in 1990–1994 and perform two flybys of large asteroids. The preferred target for this mission was Vesta. AGORA would reach the asteroid belt either by a gravitational slingshot trajectory past Mars or by means of a small ion engine. However, the proposal was refused by the ESA. A joint NASA–ESA asteroid mission was then drawn up for a Multiple Asteroid Orbiter with Solar Electric Propulsion (MAOSEP), with one of the mission profiles including an orbit of Vesta. NASA indicated they were not interested in an asteroid mission. Instead, the ESA set up a technological study of a spacecraft with an ion drive. Other missions to the asteroid belt were proposed in the 1980s by France, Germany, Italy and the United States, but none were approved.[103] Exploration of Vesta by fly-by and impacting penetrator was the second main target of the first plan of the multi-aimed Soviet Vesta mission, developed in cooperation with European countries for realisation in 1991–1994 but canceled due to the dissolution of the Soviet Union.

 
Artist's conception of Dawn orbiting Vesta

In the early 1990s, NASA initiated the Discovery Program, which was intended to be a series of low-cost scientific missions. In 1996, the program's study team recommended a mission to explore the asteroid belt using a spacecraft with an ion engine as a high priority. Funding for this program remained problematic for several years, but by 2004 the Dawn vehicle had passed its critical design review[104] and construction proceeded.[citation needed]

It launched on 27 September 2007 as the first space mission to Vesta. On 3 May 2011, Dawn acquired its first targeting image 1.2 million kilometers from Vesta.[105] On 16 July 2011, NASA confirmed that it received telemetry from Dawn indicating that the spacecraft successfully entered Vesta's orbit.[106] It was scheduled to orbit Vesta for one year, until July 2012.[107] Dawn's arrival coincided with late summer in the southern hemisphere of Vesta, with the large crater at Vesta's south pole (Rheasilvia) in sunlight. Because a season on Vesta lasts eleven months, the northern hemisphere, including anticipated compression fractures opposite the crater, would become visible to Dawn's cameras before it left orbit.[108] Dawn left orbit around Vesta on 4 September 2012 11:26 p.m. PDT to travel to Ceres.[109]

NASA/DLR released imagery and summary information from a survey orbit, two high-altitude orbits (60–70 m/pixel) and a low-altitude mapping orbit (20 m/pixel), including digital terrain models, videos and atlases.[110][111][112][113][114][115] Scientists also used Dawn to calculate Vesta's precise mass and gravity field. The subsequent determination of the J2 component yielded a core diameter estimate of about 220 km assuming a crustal density similar to that of the HED.[110]

Dawn data can be accessed by the public at the UCLA website.[116]

Observations from Earth orbit

edit
  •  
    Albedo and spectral maps of 4 Vesta, as determined from Hubble Space Telescope images from November 1994
  •  
    Elevation map of 4 Vesta, as determined from Hubble Space Telescope images of May 1996
  •  
    Elevation diagram of 4 Vesta (as determined from Hubble Space Telescope images of May 1996) viewed from the south-east, showing Rheasilvia crater at the south pole and Feralia Planitia near the equator
  •  
    Vesta seen by the Hubble Space Telescope in May 2007
  •  
    The 2006 IAU draft proposal on the definition of a planet listed Vesta as a candidate.[117] Vesta is shown fourth from the left along the bottom row.

Observations from Dawn

edit

Vesta comes into view as the Dawn spacecraft approaches and enters orbit:

  •  
    Vesta from 100,000 km
    (1 July 2011)
  •  
    Vesta from 41,000 km
    (9 July 2011)
  •  
    In orbit at 16,000 km
    (17 July 2011)
  •  
    In orbit from 10,500 km
    (18 July 2011)
  •  
    The northern hemisphere from 5,200 km
    (23 July 2011)
  •  
    In orbit from 5,200 km
    (24 July 2011)
  •  
    In orbit from 3,700 km
    (31 July 2011)
  •  
    Full rotation
    (1 August 2011)
  •  
    Composite greyscale image
  •  
    Cratered terrain with hills and ridges
    (6 August 2011)
  •  
    Densely cratered terrain near terminator
    (6 August 2011)
  •  
    Vestan craters in various states of degradation, with troughs at bottom
    (6 August 2011)
  •  
    Hill shaded central mound at the south pole of Vesta
    (2 February 2015)

True-color images

edit

Detailed images retrieved during the high-altitude (60–70 m/pixel) and low-altitude (~20 m/pixel) mapping orbits are available on the Dawn Mission website of JPL/NASA.[118]

Visibility

edit
 
Annotated image from Earth's surface in June 2007 with (4) Vesta

Its size and unusually bright surface make Vesta the brightest asteroid, and it is occasionally visible to the naked eye from dark skies (without light pollution). In May and June 2007, Vesta reached a peak magnitude of +5.4, the brightest since 1989.[119] At that time, opposition and perihelion were only a few weeks apart.[120] It was brighter still at its 22 June 2018 opposition, reaching a magnitude of +5.3.[121] Less favorable oppositions during late autumn 2008 in the Northern Hemisphere still had Vesta at a magnitude of from +6.5 to +7.3.[122] Even when in conjunction with the Sun, Vesta will have a magnitude around +8.5; thus from a pollution-free sky it can be observed with binoculars even at elongations much smaller than near opposition.[122]

2010–2011

edit

In 2010, Vesta reached opposition in the constellation of Leo on the night of 17–18 February, at about magnitude 6.1,[123] a brightness that makes it visible in binocular range but generally not for the naked eye. Under perfect dark sky conditions where all light pollution is absent it might be visible to an experienced observer without the use of a telescope or binoculars. Vesta came to opposition again on 5 August 2011, in the constellation of Capricornus at about magnitude 5.6.[123][124]

2012–2013

edit

Vesta was at opposition again on 9 December 2012.[125] According to Sky and Telescope magazine, this year Vesta came within about 6 degrees of 1 Ceres during the winter of 2012 and spring 2013.[126] Vesta orbits the Sun in 3.63 years and Ceres in 4.6 years, so every 17.4 years Vesta overtakes Ceres (the previous overtaking was in April 1996).[126] On 1 December 2012, Vesta had a magnitude of 6.6, but it had decreased to 8.4 by 1 May 2013.[126]

2014

edit
 
Conjunction of Ceres and Vesta near the star Gamma Virginis on 5 July 2014 in the Constellation of Virgo.

Ceres and Vesta came within one degree of each other in the night sky in July 2014.[126]

See also

edit

Notes

edit
  1. ^ Marc Rayman of the JPL Dawn team used "Vestian" (analogous to the Greek cognate Hestian) a few times in 2010 and early 2011 in his Dawn Journal, and the Planetary Society continued to use that form for a few more years.[2] The word had been used elsewhere, e.g. in Tsiolkovsky (1960) The call of the cosmos. However, otherwise the shorter form "Vestan" has been used by JPL.[3] Most modern print sources also use "Vestan".[4][5]
    Note that the related word "Vestalian" refers to people or things associated with Vesta, such as the vestal virgins, not to Vesta herself.
  2. ^ Calculated using the known dimensions assuming an ellipsoid.
  3. ^ Calculated using (1) the known rotation period (5.342 h)[6] and (2) the equatorial radius Req (285 km)[10] of the best-fit biaxial ellipsoid to Asteroid 4 Vesta.
  4. ^ a b topocentric coordinates computed for the selected location: Greenwich, United Kingdom[14]
  5. ^ On 10 February 2009, during Ceres perihelion, Ceres was closer to the Sun than Vesta, because Vesta has an aphelion distance greater than Ceres's perihelion distance. (10 February 2009: Vesta 2.56 AU; Ceres 2.54 AU)
  6. ^ 維斯塔 wéisītǎ is the closest Chinese approximation of the Latin pronunciation westa.
  7. ^ Some sources contemporaneous to Gauss invented more elaborate forms, such as   and  .[45][46] A simplification of the latter from c. 1930,  ,[47] never caught on.
  8. ^ This symbol can be seen in the top of the most elaborate of the earlier forms,  . It dates from 1973, at the beginning of astrological interest in asteroids.[48]
  9. ^ The data returned will include, for both asteroids, full surface imagery, full surface spectrometric mapping, elemental abundances, topographic profiles, gravity fields, and mapping of remnant magnetism, if any.[55]
  10. ^ that is, blue in the north does not mean the same thing as blue in the south.
  11. ^ Note that there is very strong evidence that 6 Hebe is the parent body for H-chondrites, one of the most common meteorite types.

References

edit
  1. ^ "Vesta". Dictionary.com Unabridged (Online). n.d.
  2. ^ "Search Results". Planetary Society. Archived from the original on 27 July 2020. Retrieved 31 August 2012.
  3. ^ "Search��– Dawn Mission". JPL. Archived from the original on 5 March 2016.
  4. ^ Meteoritics & planetary science, Volume 42, Issues 6–8, 2007; Origin and evolution of Earth, National Research Council et al., 2008
  5. ^ E.g in Meteoritics & planetary science (volume 42, issues 6–8, 2007) and Origin and evolution of Earth (National Research Council et al., 2008).
  6. ^ a b c d e f g h "JPL Small-Body Database Browser: 4 Vesta". Archived from the original on 26 September 2021. Retrieved 1 June 2008.
  7. ^ 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.
  8. ^ "Horizons Batch for 4 Vesta on 2021-Dec-26" (Perihelion occurs when rdot flips from negative to positive). JPL Horizons. Retrieved 26 September 2021. (Epoch 2021-Jul-01/Soln.date: 2021-Apr-13)
  9. ^ "AstDyS-2 Vesta Synthetic Proper Orbital Elements". Department of Mathematics, University of Pisa, Italy. Retrieved 1 October 2011.
  10. ^ a b c d e f g h i Russell, C. T.; et al. (2012). "Dawn at Vesta: Testing the Protoplanetary Paradigm" (PDF). Science. 336 (6082): 684–686. Bibcode:2012Sci...336..684R. doi:10.1126/science.1219381. PMID 22582253. S2CID 206540168.
  11. ^ "surface ellipsoid 286.3x278.6x223.2". Wolfram-Alpha: Computational Knowledge Engine.
  12. ^ Konopliv, A. S.; et al. (2014). "The Vesta gravity field, spin pole and rotation period, landmark positions, and ephemeris from the Dawn tracking and optical data". Icarus. 240: 118–132. Bibcode:2014Icar..240..103K. doi:10.1016/j.icarus.2013.09.005. PDF copy
  13. ^ Harris, A. W. (2006). Warner, B. D.; Pravec, P. (eds.). "Asteroid Lightcurve Derived Data. EAR-A-5-DDR-DERIVED-LIGHTCURVE-V8.0". NASA Planetary Data System. Archived from the original on 9 April 2009. Retrieved 26 December 2013.
  14. ^ "Asteroid 4 Vesta". TheSkyLive. Retrieved 13 December 2022.
  15. ^ a b Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (2004). "Infra-Red Astronomy Satellite (IRAS) Minor Planet Survey. IRAS-A-FPA-3-RDR-IMPS-V6.0". NASA Planetary Data System. Archived from the original on 9 April 2009. Retrieved 15 March 2007.
  16. ^ a b Mueller, T. G.; Metcalfe, L. (2001). "ISO and Asteroids" (PDF). ESA Bulletin. 108: 38. Bibcode:2001ESABu.108...39M. Archived (PDF) from the original on 11 September 2005.
  17. ^ Neese, C.; Ed. (2005). "Asteroid Taxonomy EAR-A-5-DDR-TAXONOMY-V5.0". NASA Planetary Data System. Archived from the original on 10 March 2007. Retrieved 25 December 2013.
  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. ^ "In Depth - 4 Vesta". NASA Solar System Exploration. Retrieved 13 December 2022.
  20. ^ "Dawn Mission Overview". NASA. Archived from the original on 16 October 2011. Retrieved 14 August 2011.
  21. ^ Lang, Kenneth (2011). The Cambridge Guide to the Solar System. Cambridge University Press. pp. 372, 442. ISBN 9780521198578.
  22. ^ Russell, C. T.; et al. (2011). "Exploring the smallest terrestrial planet: Dawn at Vesta" (PDF). EPSC Abstracts. 2011 EPSC-DPS Joint Meeting. Vol. 6. EPSC-DPS2011-97-3. Archived (PDF) from the original on 20 March 2012.
  23. ^ a b Pitjeva, E. V. (2005). "High-Precision Ephemerides of Planets—EPM and Determination of Some Astronomical Constants" (PDF). Solar System Research. 39 (3): 176–186. Bibcode:2005SoSyR..39..176P. doi:10.1007/s11208-005-0033-2. S2CID 120467483. Archived from the original (PDF) on 31 October 2008.
  24. ^ a b Savage, Don; Jones, Tammy & Villard, Ray (19 April 1995). "Asteroid or Mini-Planet? Hubble Maps the Ancient Surface of Vesta" (Press release). HubbleSite. News Release STScI-1995-20. Retrieved 17 October 2006.
  25. ^ a b "A look into Vesta's interior". Max-Planck-Gesellschaft. 6 January 2011.
  26. ^ "Asteroid Vesta is "last of a kind" rock". BBC, 11 May 2012.
  27. ^ Jutzi, M.; E. Asphaug; P. Gillet; J.-A. Barrat; W. Benz (14 February 2013). "The structure of the asteroid 4 Vesta as revealed by models of planet-scale". Nature. 494 (7436): 207–210. Bibcode:2013Natur.494..207J. doi:10.1038/nature11892. PMID 23407535. S2CID 4410838.
  28. ^ Cook, Jia-Rui. "Dawn Reality-Checks Telescope Studies of Asteroids". Archived from the original on 2 May 2014. Retrieved 30 April 2014.
  29. ^ McSween, H. Y.; R. P. Binzel; M. C. De Sanctis; et al. (27 November 2013). "Dawn; the Vesta-HED connection; and the geologic context for eucrite, diogenites, and howardites". Meteoritics & Planetary Science. 48 (11): 2090–21–4. Bibcode:2013M&PS...48.2090M. doi:10.1111/maps.12108. S2CID 131100157.
  30. ^ a b Kelley, M. S.; et al. (2003). "Quantified mineralogical evidence for a common origin of 1929 Kollaa with 4 Vesta and the HED meteorites". Icarus. 165 (1): 215–218. Bibcode:2003Icar..165..215K. doi:10.1016/S0019-1035(03)00149-0.
  31. ^ a b "Vesta". NASA/JPL. 12 July 2011. Archived from the original on 29 June 2011. Retrieved 30 July 2011.
  32. ^ "Ceres, Pallas, Vesta, and Hygiea". Gravity Simulator. Archived from the original on 17 June 2008. Retrieved 31 May 2008.
  33. ^ "Mission > Mission Status – Dawn Mission". JPL. Archived from the original on 11 May 2013. Retrieved 6 September 2012.
  34. ^ a b Ammannito, E.; M. C. De Sanctis; E. Palomba; et al. (2013). "Olivine in an unexpected location on Vesta's surface". Nature. 504 (7478): 122–125. Bibcode:2013Natur.504..122A. doi:10.1038/nature12665. PMID 24196707. S2CID 4464889.
  35. ^ Cook, Jia-Rui. "It's Complicated: Dawn Spurs Rewrite of Vesta's Story". Archived from the original on 2 May 2014. Retrieved 30 April 2014.
  36. ^ Littmann, Mark (2004). Planets Beyond: Discovering the Outer Solar System. Dover Books on Astronomy. Courier Dover Publications. p. 21. ISBN 978-0-486-43602-9.
  37. ^ Lynn, W. T. (February 1907). "The discovery of Vesta". The Observatory. 30: 103–105. Bibcode:1907Obs....30..103L.
  38. ^ Dunnington, Guy Waldo; Gray, Jeremy; Dohse, Fritz-Egbert (2004). Carl Friedrich Gauss: Titan of Science. The Mathematical Association of America. p. 76. ISBN 978-0-88385-547-8.
  39. ^ Rao, K. S.; Berghe, G. V. (2003). "Gauss, Ramanujan and Hypergeometric Series Revisited". Historia Scientiarum. 13 (2): 123–133.
  40. ^ Schmadel, Lutz D. (2003). Dictionary of Minor Planet Names: Prepared on Behalf of Commission 20 Under the Auspices of the International Astronomical Union. Springer. p. 15. ISBN 978-3-540-00238-3.
  41. ^ von Zach, Franz Xaver (1807). Monatliche correspondenz zur beförderung der erd- und himmels-kunde. Vol. 15. p. 507.
  42. ^ Carlini, Francesco (1808). Effemeridi astronomiche di Milano per l'anno 1809.
  43. ^ a b Bala, Gavin Jared; Miller, Kirk (18 September 2023). Unicode request for historical asteroid symbols (PDF) (Report). Unicode Consortium. Retrieved 26 September 2023 – via unicode.org.
  44. ^ "Proposed new characters". unicode.org. The Pipeline. Unicode Consortium. Retrieved 6 November 2023.
  45. ^ Bureau des longitudes (1807). Annuaire pour l'an 1808. p. 5.
  46. ^ Canovai, Stanislao; del-Ricco, Gaetano (1810). Elementi di fisica matematica. p. 149.
  47. ^ Koch, Rudolf (1955) [1930]. The Book of Signs (reprint ed.). Dover.
  48. ^ Bach, Eleanor (1973). Ephemerides of the asteroids: Ceres, Pallas, Juno, Vesta, 1900–2000. Celestial Communications.
  49. ^ Wells, David A. (1851). Bliss, George Jr. (ed.). "The Planet Hygiea". Annual of Scientific Discovery for the year 1850, quoted by spaceweather.com archives, 2006-09-13. Retrieved 1 June 2008.
  50. ^ Hilton, James L. When Did the Asteroids Become Minor Planets? (Report). Archived from the original on 24 March 2008 – via U.S. Naval Observatory website, particularly the discussion of Gould, B. A. (1852). "On the Symbolic Notation of the Asteroids". Astronomical Journal. 2: 80. Bibcode:1852AJ......2...80G. doi:10.1086/100212. and immediate subsequent history. Also, the discussion of C. J. Cunningham (1988) Introduction to Asteroids explains the parenthetical part.
  51. ^ "New SPHERE view of Vesta". www.eso.org. Retrieved 25 June 2018.
  52. ^ McFadden, L. A.; Emerson, G.; Warner, E. M.; Onukwubiti, U.; Li, J.-Y. "Photometry of 4 Vesta from its 2007 Apparition". Proceedings, 39th Lunar and Planetary Science Conference. League City, Texas. Bibcode:2008LPI....39.2546M. 10–14 March 2008
  53. ^ Hughes, D. W. (September 1994). "The Historical Unravelling of the Diameters of the First Four Asteroids". Quarterly Journal of the Royal Astronomical Society. 35 (3): 331. Bibcode:1994QJRAS..35..331H.
  54. ^ Povenmire, H. (September 2001). "The January 4, 1991 Occultation of SAO 93228 by Asteroid (4) Vesta". Meteoritics & Planetary Science. 36 (Supplement): A165. Bibcode:2001M&PSA..36Q.165P. doi:10.1111/j.1945-5100.2001.tb01534.x.
  55. ^ a b "Dawn-NASA-NSSDCA-Spacecraft-Details". Archived from the original on 23 May 2022. Retrieved 16 December 2022.
  56. ^ Hertz, Hans G. (19 April 1968). "Mass of Vesta". Science. 160 (3825): 299–300. Bibcode:1968Sci...160..299H. doi:10.1126/science.160.3825.299. PMID 17788233. S2CID 2555834.
  57. ^ Kovačević, A. (January 2005). "Determination of the mass of (4) Vesta based on new close approaches". Astronomy and Astrophysics. 430 (1): 319–325. Bibcode:2005A&A...430..319K. doi:10.1051/0004-6361:20035872.
  58. ^ Christou, A. A. (2000). "Co-orbital objects in the main asteroid belt". Astronomy and Astrophysics. 356: L71–L74. Bibcode:2000A&A...356L..71C.
  59. ^ a b Christou, A. A.; Wiegert, P. (January 2012). "A population of Main Belt Asteroids co-orbiting with Ceres and Vesta". Icarus. 217 (1): 27–42. arXiv:1110.4810. Bibcode:2012Icar..217...27C. doi:10.1016/j.icarus.2011.10.016. ISSN 0019-1035. S2CID 59474402.
  60. ^ a b c Thomas, P. C.; et al. (1997). "Vesta: Spin Pole, Size, and Shape from HST Images". Icarus. 128 (1): 88–94. Bibcode:1997Icar..128...88T. doi:10.1006/icar.1997.5736.
  61. ^ a b Hand, Eric (2012). "Space missions trigger map wars". Nature. 488 (7412): 442–443. Bibcode:2012Natur.488..442H. doi:10.1038/488442a. PMID 22914145.
  62. ^ "IAU WGCCRE Coordinate System for Vesta | USGS Astrogeology Science Center". Astrogeology.usgs.gov. 15 November 2013. Retrieved 25 June 2014.
  63. ^ Li, Jian-Yang; Mafi, Joseph N. "Body-Fixed Coordinate Systems for Asteroid (4) Vesta" (PDF). Planetary Data System. Archived (PDF) from the original on 6 November 2015.
  64. ^ Baer, James; Chesley, Steven R. (2008). "Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris". Celestial Mechanics and Dynamical Astronomy. 100 (1): 27–42. Bibcode:2008CeMDA.100...27B. doi:10.1007/s10569-007-9103-8.
  65. ^ Carry, B.; et al. (2009). "Physical properties of (2) Pallas". Icarus. 205 (2): 460–472. arXiv:0912.3626v1. Bibcode:2010Icar..205..460C. doi:10.1016/j.icarus.2009.08.007. S2CID 119194526.
  66. ^ "The IAU draft definition of "planet" and "plutons"". IAU. August 2006. Archived from the original on 9 January 2010. Retrieved 16 December 2009. (XXVI)
  67. ^ Fu, R. R.; Hager, B. H.; Ermakov, A.I.; Zuber, M.T. (2013). "Early Viscous Relaxation of Asteroid Vesta and Implications for Late Impact-Driven Despinning" (PDF). 44th Lunar and Planetary Science Conference (1719): 2115. Bibcode:2013LPI....44.2115F. Archived (PDF) from the original on 26 July 2014.
  68. ^ Asmar, S. W.; Konopliv, A. S.; Park, R. S.; et al. (2012). "The Gravity Field of Vesta and Implications for Interior Structure" (PDF). 43rd Lunar and Planetary Science Conference (1659): 2600. Bibcode:2012LPI....43.2600A. Archived (PDF) from the original on 20 October 2013.
  69. ^ Zellner, N. E. B.; Gibbard, S.; de Pater, I.; et al. (2005). "Near-IR imaging of Asteroid 4 Vesta" (PDF). Icarus. 177 (1): 190–195. Bibcode:2005Icar..177..190Z. doi:10.1016/j.icarus.2005.03.024. Archived from the original (PDF) on 23 November 2008.
  70. ^ Jaumann, R.; et al. (2012). "Vesta's Shape and Morphology". Science. 336 (6082): 687–690. Bibcode:2012Sci...336..687J. doi:10.1126/science.1219122. PMID 22582254. S2CID 206540010.
  71. ^ a b c Williams, D. A.; Yingst, R. A.; Garry, W. B. (December 2014). "Introduction: The geologic mapping of Vesta". Icarus. 244: 1–12. Bibcode:2014Icar..244....1W. doi:10.1016/j.icarus.2014.03.001. hdl:2286/R.I.28071.
    —Williams, D. A.; et al. (December 2014). "The geology of the Marcia quadrangle of asteroid Vesta: Assessing the effects of large, young craters". Icarus. 244: 74–88. Bibcode:2014Icar..244...74W. doi:10.1016/j.icarus.2014.01.033. hdl:2286/R.I.28061. S2CID 5505009.
  72. ^ a b Scully, J. E. C.; Yin, A.; Russell, C. T.; et al. (December 2014). "Geomorphology and structural geology of Saturnalia Fossae and adjacent structures in the northern hemisphere of Vesta". Icarus. 244: 23–40. Bibcode:2014Icar..244...23S. doi:10.1016/j.icarus.2014.01.013. hdl:2286/R.I.28070. Archived (PDF) from the original on 21 July 2018.
    —Scully, J. E. C.; et al. (2014). "Sub-curvilinear gullies interpreted as evidence for transient water flow on Vesta" (PDF). 45th Lunar and Planetary Science Conference (1777): 1796. Bibcode:2014LPI....45.1796S.
  73. ^ Schäfer, M.; Nathues, A.; Williams, D. A.; et al. (December 2014). "Imprint of the Rheasilvia impact on Vesta – Geologic mapping of quadrangles Gegania and Lucaria" (PDF). Icarus. 244: 60–73. Bibcode:2014Icar..244...60S. doi:10.1016/j.icarus.2014.06.026. hdl:2286/R.I.28060. Archived from the original (PDF) on 28 April 2019. Retrieved 24 September 2019.
  74. ^ Kneissl, T.; Schmedemann, N.; Reddy, V.; et al. (December 2014). "Morphology and formation ages of mid-sized post-Rheasilvia craters – Geology of quadrangle Tuccia, Vesta". Icarus. 244: 133–157. Bibcode:2014Icar..244..133K. doi:10.1016/j.icarus.2014.02.012. hdl:2286/R.I.28058.
  75. ^ a b c Schenk, P.; et al. (2012). "The Geologically Recent Giant Impact Basins at Vesta's South Pole". Science. 336 (6082): 694–697. Bibcode:2012Sci...336..694S. doi:10.1126/science.1223272. PMID 22582256. S2CID 206541950.
  76. ^ "Rheasilvia – Super Mysterious South Pole Basin at Vesta is Named after Romulus and Remus Roman Mother". Universe Today. 21 September 2011. Retrieved 23 September 2011.
  77. ^ Binzel, R. P.; et al. (1997). "Geologic Mapping of Vesta from 1994 Hubble Space Telescope Images". Icarus. 128 (1): 95–103. Bibcode:1997Icar..128...95B. doi:10.1006/icar.1997.5734.
  78. ^ Karimi, S; Dombard, A.J. (2016). "On the possibility of viscoelastic deformation of the large south polar craters and true polar wander on the asteroid Vesta". Journal of Geophysical Research. 121 (9): 1786–1797. Bibcode:2016JGRE..121.1786K. doi:10.1002/2016JE005064.
  79. ^ Garry, W.B.; Sykes, M.; Buczkowski, D.L.; et al. (March 2012). Geologic Mapping of Av-10 Oppia Quadrangle of Asteroid 4 Vesta (PDF). 43rd Lunar and Planetary Science Conference, held 19–23 March 2012 at The Woodlands, Texas. id.2315. Bibcode:2012LPI....43.2315G. LPI Contribution No. 1659. Archived (PDF) from the original on 24 April 2014.
    —Garry, W.B.; Sykes, M.; Buczkowski, D.L.; et al. (April 2012). "Geologic Mapping of Av-10 Oppia Quadrangle of Asteroid 4 Vesta" (PDF). Geophysical Research Abstracts. EGU General Assembly 2012, held 22–27 April 2012 in Vienna, Austria. Vol. 14. p. 5711. Bibcode:2012EGUGA..14.5711G. EGU2012-5711-1. Archived (PDF) from the original on 8 April 2014.
  80. ^ "Nomenclature Search Results / Target: VESTA / Feature Type: Crater, craters". Gazetteer of Planetary Nomenclature. IAU.
  81. ^ Beatty, J. Kelly (25 June 2004). "Eros's puzzling surface". Sky and Telescope. Retrieved 18 October 2023 – via skyandtelescope.org. To geologists' surprise, the asteroid Eros has more than 250 'ponds' thought to contain compacted deposits of finely ground dust.
  82. ^ Parekh, R.; Otto, K.A.; Matz, K.D.; Jaumann, R.; Krohn, K.; Roatsch, T.; et al. (28 February 2022) [1 November 2021]. "Formation of ejecta and dust pond deposits on asteroid Vesta". Journal of Geophysical Research: Planets. 126 (11): e2021JE006873. doi:10.1029/2021JE006873. Retrieved 18 October 2023 – via agupubs.onlinelibrary.
  83. ^ Buczkowski, D.L.; Raymond, C.A.; Williams, D.A.; et al. (2012). "Large-scale troughs on Vesta: A signature of planetary tectonics". Geophysical Research Letters. 39 (18): L18205. Bibcode:2012GeoRL..3918205B. doi:10.1029/2012GL052959.
  84. ^ "Asteroid's troughs suggest stunted planet" (Press release). American Geophysical Union. 26 September 2012. AGU Release No. 12-42. Archived from the original on 29 September 2012. Retrieved 25 November 2012.
  85. ^ Hirata, N. (2023). "Secondary Cratering From Rheasilvia as the Possible Origin of Vesta's Equatorial Troughs". Retrieved 4 March 2024.
  86. ^ De Sanctis, M. C.; et al. (2012). "Spectroscopic Characterization of Mineralogy and Its Diversity Across Vesta". Science. 336 (6082): 697–700. Bibcode:2012Sci...336..697D. doi:10.1126/science.1219270. PMID 22582257. S2CID 11645621.
  87. ^ Prettyman, T. H.; et al. (2012). "Elemental Mapping by Dawn Reveals Exogenic H in Vesta's Regolith". Science. 338 (6104): 242–246. Bibcode:2012Sci...338..242P. doi:10.1126/science.1225354. PMID 22997135. S2CID 206542798.
  88. ^ a b Reddy, V.; et al. (2012). "Color and Albedo Heterogeneity of Vesta from Dawn". Science. 336 (6082): 700–704. Bibcode:2012Sci...336..700R. doi:10.1126/science.1219088. PMID 22582258. S2CID 1326996.
  89. ^ Palomba, E.; Longobardo, A.; De Sanctis, M. C.; et al. (September 2015). "Detection of new olivine-rich locations on Vesta". Icarus. 258: 120–134. Bibcode:2015Icar..258..120P. doi:10.1016/j.icarus.2015.06.011.
  90. ^ Denevi, B. W.; et al. (2012). "Pitted Terrain on Vesta and Implications for the Presence of Volatiles". Science. 338 (6104): 246–249. Bibcode:2012Sci...338..246D. CiteSeerX 10.1.1.656.1476. doi:10.1126/science.1225374. PMID 22997131. S2CID 22892716.
  91. ^ De Sanctis, M. C.; et al. (2012). "Detection of Widespread Hydrated Materials on Vesta by the vir Imaging Spectrometer on Board Thedawnmission". The Astrophysical Journal Letters. 758 (2): L36. Bibcode:2012ApJ...758L..36D. doi:10.1088/2041-8205/758/2/L36.
  92. ^ Ghosh, A.; McSween, H. Y. (1998). "A Thermal Model for the Differentiation of Asteroid 4 Vesta, Based on Radiogenic Heating". Icarus. 134 (2): 187–206. Bibcode:1998Icar..134..187G. doi:10.1006/icar.1998.5956.
  93. ^ Righter, K.; Drake, M. J. (1997). "A magma ocean on Vesta: Core formation and petrogenesis of eucrites and diogenites". Meteoritics & Planetary Science. 32 (6): 929–944. Bibcode:1997M&PS...32..929R. doi:10.1111/j.1945-5100.1997.tb01582.x. S2CID 128684062.
  94. ^ Drake, M. J. (2001). "The eucrite/Vesta story". Meteoritics & Planetary Science. 36 (4): 501–513. Bibcode:2001M&PS...36..501D. doi:10.1111/j.1945-5100.2001.tb01892.x. S2CID 128394153.
  95. ^ Sahijpal, S.; Soni, P.; Gagan, G. (2007). "Numerical simulations of the differentiation of accreting planetesimals with 26Al and 60Fe as the heat sources". Meteoritics & Planetary Science. 42 (9): 1529–1548. Bibcode:2007M&PS...42.1529S. doi:10.1111/j.1945-5100.2007.tb00589.x. S2CID 55463404.
  96. ^ Gupta, G.; Sahijpal, S. (2010). "Differentiation of Vesta and the parent bodies of other achondrites". J. Geophys. Res. Planets. 115 (E8): E08001. Bibcode:2010JGRE..115.8001G. doi:10.1029/2009JE003525. S2CID 129905814.
  97. ^ Cook, Jia-Rui C. (29 March 2011). "When Is an Asteroid Not an Asteroid?". NASA/JPL. Archived from the original on 29 June 2011. Retrieved 30 July 2011.
  98. ^ Takeda, H. (1997). "Mineralogical records of early planetary processes on the HED parent body with reference to Vesta". Meteoritics & Planetary Science. 32 (6): 841–853. Bibcode:1997M&PS...32..841T. doi:10.1111/j.1945-5100.1997.tb01574.x.
  99. ^ Yamaguchi, A.; Taylor, G. J.; Keil, K. (1995). "Metamorphic History of the Eucritic Crust of 4 Vesta". Meteoritical Society. 30 (5): 603. Bibcode:1995Metic..30..603Y.
  100. ^ Pieters, C. M.; Ammannito, E.; Blewett, D. T.; et al. (2012). "Distinctive space weathering on Vesta from regolith mixing processes". Nature. 491 (7422): 79–82. Bibcode:2012Natur.491...79P. doi:10.1038/nature11534. PMID 23128227. S2CID 4407636.
  101. ^ McCord, T. B.; Li, J. -Y.; Combe, J. -P.; et al. (2012). "Dark material on Vesta from the infall of carbonaceous volatile-rich material". Nature. 491 (7422): 83–86. Bibcode:2012Natur.491...83M. doi:10.1038/nature11561. PMID 23128228. S2CID 2058249.
  102. ^ Rayman, Marc (8 April 2015). Now Appearing At a Dwarf Planet Near You: NASA's Dawn Mission to the Asteroid Belt (Speech). Silicon Valley Astronomy Lectures. Foothill College, Los Altos, CA. Archived from the original on 14 November 2021. Retrieved 7 July 2018.
  103. ^ Ulivi, Paolo; Harland, David (2008). Robotic Exploration of the Solar System: Hiatus and Renewal, 1983–1996. Springer Praxis Books in Space Exploration. Springer. pp. 117–125. ISBN 978-0-387-78904-0.
  104. ^ Russell, C. T.; Capaccioni, F.; Coradini, A.; et al. (October 2007). "Dawn Mission to Vesta and Ceres" (PDF). Earth, Moon, and Planets. 101 (1–2): 65–91. Bibcode:2007EM&P..101...65R. doi:10.1007/s11038-007-9151-9. S2CID 46423305. Archived (PDF) from the original on 27 September 2011. Retrieved 13 June 2011.
  105. ^ Cook, Jia-Rui C.; Brown, Dwayne C. (11 May 2011). "NASA's Dawn Captures First Image of Nearing Asteroid". NASA/JPL. Archived from the original on 29 January 2012. Retrieved 14 May 2011.
  106. ^ Vega, Priscilla; Brown, Dwayne (16 July 2011). "NASA's Dawn Spacecraft Enters Orbit Around Asteroid Vesta". NASA. Archived from the original on 19 June 2012. Retrieved 17 July 2011.
  107. ^ Dawn mission timeline Archived 19 October 2013 at the Wayback Machine
  108. ^ Mid-continent Research for Education and Learning: McREL (27 September 2010). "Dawn Mission: Mission". Dawn Journal. Retrieved 29 March 2011.
  109. ^ "Dawn has Departed the Giant Asteroid Vesta". NASA JPL. NASA. 5 September 2012. Retrieved 5 September 2012.
  110. ^ a b Russell, C. T.; et al. (2013). "Dawn completes its mission at 4 Vesta". Meteoritics & Planetary Science. 48 (11): 2076–2089. Bibcode:2013M&PS...48.2076R. doi:10.1111/maps.12091.
  111. ^ Roatsch, Thomas; et al. (2012). "High resolution Vesta High Altitude Mapping Orbit (HAMO) Atlas derived from Dawn framing camera images". Planetary and Space Science. 73 (1): 283–286. Bibcode:2012P&SS...73..283R. doi:10.1016/j.pss.2012.08.021.
  112. ^ Roatsch, Thomas; et al. (2013). "High-resolution Vesta Low Altitude Mapping Orbit Atlas derived from Dawn Framing Camera images". Planetary and Space Science. 85: 293–298. Bibcode:2013P&SS...85..293R. doi:10.1016/j.pss.2013.06.024.
  113. ^ "NASA's Journey Above Vesta". DLR Institute of Planetary Research video with NASA JPL imagery. NASA. 16 September 2011. Archived from the original on 22 April 2021. Retrieved 18 September 2011.
  114. ^ "DLR public Dawn products site". Archived from the original on 16 October 2015.
  115. ^ "NASA Dawn".
  116. ^ "Dawn Public Data". Dawn [website]. Univ. California, Los Angeles. Retrieved 6 March 2015.
  117. ^ Gingerich, Owen (2006). "The Path to Defining Planets" (PDF). Dissertatio cum Nuncio Sidereo Ill. Tertia. Vol. VIII, no. 16. pp. 4–5. Archived (PDF) from the original on 15 March 2015. Retrieved 13 March 2007.
  118. ^ "Dawn Mission website of JPL/NASA".
  119. ^ Bryant, Greg (2007). "Sky & Telescope: See Vesta at Its Brightest!". Retrieved 7 May 2007.
  120. ^ "Vesta Finder". Sky & Telescope. Archived from the original on 12 June 2007. Retrieved 7 May 2007.
  121. ^ Harrington, Philip S. (21 October 2010). Cosmic Challenge: The Ultimate Observing List for Amateurs. Cambridge University Press. p. 75. ISBN 9781139493680.
  122. ^ a b James, Andrew (2008). "Vesta". Southern Astronomical Delights. Retrieved 6 November 2008.
  123. ^ a b Yeomans, Donald K.; Chamberlin, Alan B. "Horizons Ephemeris". JPL Solar System Dynamics. Retrieved 9 January 2010.
  124. ^ "Elements and Ephemeris for (4) Vesta". Minor Planet Center. Archived from the original on 4 March 2016.
  125. ^ "2012 Astronomy Special". Nightskyonline.info. Archived from the original on 20 April 2012. Retrieved 23 November 2012.
  126. ^ a b c d T. Flanders – Ceres and Vesta: July 2012 – April 2013 – Sky & Telescope.

Bibliography

edit
  • The Dawn Mission to Minor Planets 4 Vesta and 1 Ceres, Christopher T. Russell and Carol A. Raymond (Editors), Springer (2011), ISBN 978-1-4614-4903-4
  • Keil, K.; Geological History of Asteroid 4 Vesta: The Smallest Terrestrial Planet in Asteroids III, William Bottke, Alberto Cellino, Paolo Paolicchi, and Richard P. Binzel, (Editors), University of Arizona Press (2002), ISBN 0-8165-2281-2
edit
 
Wikimedia Commons has media related to Vesta (asteroid).
This video explores Vesta's landscape, history and planet-like characteristics.
Retrieved from "https://en.wikipedia.org/w/index.php?title=4_Vesta&oldid=1255637206"