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4 Vesta seen by Dawn spacecraft July 9, 2011
|Discovered by||Heinrich Wilhelm Olbers|
|Discovery time||March 29, 1807|
|Group||Main belt (Vesta family)|
|Reference date November 26, 2005 (JD 2453700.5)|
|Longest distance from the Sun||384.72 Gm (2.572 AU)|
|Shortest distance from the Sun||321.82 Gm (2.151 AU)|
|Longest distance from the center of its orbital path
|353.268 Gm (2.361 AU)|
|How egg-shaped its orbit is
|How long it takes to complete an orbit||1325.46 d (3.63 a)|
|Average speed||19.34 km/s|
|Angle above the reference plane
|Longitude of where it comes up through the reference plane||103.926°|
|Angle between its shortest distance from what it orbits around and where it comes up through the reference plane
("argument of periapsis")
|Size and Other Qualities|
|Average density||3.4 g/cm³|
|Gravity at its surface||0.22 m/s²|
|Slowest speed able to escape into space
|How long it takes to turn around one time||0.2226 d|
|How much light it reflects||0.423 (geometric)|
|Avg. surface temp.||
min: 85 K (-188° C)|
max: 255 K (-18 °C)
|5.1 to 8.48|
|0.64" to 0.20"|
4 Vesta (IPA: [ˈvɛstə]) is the second most massive asteroid in the solar system, with an average diameter of about 530 km (around 330 miles) and an estimated mass 9% the mass of the entire asteroid belt. Vesta's astronomical symbol is .
Vesta was discovered by the German astronomer Heinrich Wilhelm Olbers on March 29, 1807. He allowed the prominent mathematician Carl Friedrich Gauss to name the asteroid after the Roman virgin goddess of home and hearth, Vesta.
After the discovery of Vesta in 1807, no asteroids were discovered for the next 38 years. During this time the four known asteroids were counted among the planets, and each had its own planetary symbol. Vesta was normally represented by a stylized hearth (). Other symbols are and . All are simplifications of the original .
Vesta is the second-most massive body in the asteroid belt. Vesta does have a different interior compared to its surface. It is in the Inner Main Belt, at a distance of about 2.50 AU. It is similar to 2 Pallas in volume (although it is not confirmed), but somewhat more massive.
Vesta's shape is close to the shape of a sphere by its own gravity, but the large concavity and lump at the pole (see 'Surface Features' below) did not fit the criteria from being considered a planet under the IAU. In any case, this resolution was rejected by the IAU membership and Vesta will continue to be called an asteroid. However, it is possible that Vesta may be listed as a dwarf planet in the future, if it is convincingly determined that its shape is from hydrostatic equilibrium.
Its rotation is actually 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° with an uncertainty of about 10°. This gives an axial tilt of 29°.
Temperatures on the surface have been thought to be between about -20°C with the Sun overhead, dropping to about -190°C at the winter pole. Typical day-time and night-time temperatures are -60°C and -130°C, respectively. This estimate is for May 6, 1996, very close to perihelion, while details vary somewhat with the seasons.
Vesta is thought to consist of a metallic iron-nickel core, above with a rocky olivine mantle, and a surface crust. From the first appearance of Ca-Al-rich inclusions (the first solid matter in the Solar System, forming about 4567 million years ago), a likely timeline is as follows:
- Accretion completed after about 2-3 million years.
- Complete or almost complete melting due to radioactive decay of 26Al, leading to separation of the metal core at about 4-5 million years.
- Progressive crystallization of a convecting molten mantle. Convection stopped when about 80% of the material had crystallized, at about 6-7 million years.
- 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, while 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 procedure. 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 broken by impacts.
The most notable surface feature is a very large crater that is 460 km in diameter centered near the south pole. Its width is about 80% of the entire diameter of Vesta. The floor of this crater is about 13 km below, and its rim rises 4–12 km above the surrounding area, with total surface relief of about 25 km. A central peak rises 18 km above the crater floor. It is thought that the impact responsible blew up about 1% of the entire volume of Vesta, and it is likely that a group of smaller asteroids known as the Vesta family are the remains of this collision. If this is the case, then the fact that 10 km fragments of the Vesta family have survived bombardment until the present indicates that the crater is only about 1 billion years old or younger. It would also be the original site of origin of the HED meteorites. In fact, 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 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 which is indicated by spectral signatures of olivine. Interestingly Vesta was not disrupted nor resurfaced by an impact of this magnitude.
Several other large craters about 150 km wide and 7 km deep are also present. A dark feature about 200 km across has been named Olbers in honour of Vesta's discoverer, but it does not appear in elevation maps as a fresh crater would, and its nature is presently unknown, perhaps an old basaltic surface. It serves as a reference point with the 0° longitude prime meridian defined to pass through its center.
The eastern and western hemispheres show markedly different terrains. From preliminary spectral analyses of the Hubble Space Telescope images, the eastern hemisphere appears to be have a highly reflective, heavily cratered "highland" terrain with old, dusty rocks, and craters probing into deeper plutonic layers of the crust. On the other hand, large regions of the western hemisphere are taken up by dark geologic units thought to be surface basalts.
Various small solar system objects are believed to be fragments of Vesta caused by collisions. The Vestoid 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.
Because a number of meteorites are believed to be Vestian fragments, Vesta is currently one of only five identified Solar system bodies for which we have physical samples, the others being Mars, the Moon, comet Wild 2, and Earth itself.
Proof of HED meteorite origin
Vesta is the source of the HED meteorites, which are about 6% of all the meteorites which fall to Earth. These meteorites have pyroxene, which is a mineral rich in iron and magnesium. This has been matched exactly to the mineral signatures on Vesta's surface captured by Dawn's instruments.
Its size and unusually bright surface make Vesta the brightest asteroid, and it is occasionally visible to the eye from dark (non-light polluted) skies. Recently, in May and June 2007, Vesta reached a peak magnitude of +5.4, the brightest since 1989.
Less favourable oppositions during late autumn in the Northern Hemisphere still have Vesta at a magnitude of around +7.0. 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.
- P. C. Thomas et al. Impact excavation on asteroid 4 Vesta: Hubble Space Telescope results, Science, Vol. 277, pp. 1492 (1997).
- 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 - July 25, 2004, in Paris, France : 2014.
- Harris, A. W.; Warner, B.D.; Pravec, P.; Eds. (2006). "Asteroid Lightcurve Derived Data. EAR-A-5-DDR-DERIVED-LIGHTCURVE-V8.0.". NASA Planetary Data System. http://www.psi.edu/pds/resource/lc.html. Retrieved 2007-3-15.
- 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. http://www.psi.edu/pds/resource/imps.html. Retrieved 2007-03-15.
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- Neese, C.; Ed. (2005). "Asteroid Taxonomy.EAR-A-5-DDR-TAXONOMY-V5.0.". NASA Planetary Data System. http://www.psi.edu/pds/resource/taxonomy.html. Retrieved 2007-3-15.
- Donald H. Menzel and Jay M. Pasachoff (1983). A Field Guide to the Stars and Planets (2nd edition ed.). Boston, MA: Houghton Mifflin. pp. p. 391. .
- Older form and discussion of its complexity from Gould, 1852. Gould, B.A. 1852, On the Symbolic Notation of the Asteroids, Astron. J., 2, as cited and discussed here.
- Key Stages in the Evolution of the Asteroid Vesta, Hubble Space Telescope news release, April 19 (1995)
- P. C. Thomas et al. Vesta: Spin Pole, Size, and Shape from HST Images, Icarus, Vol. 128, p. 88 (1997).
- A. Ghosh and H. Y. McSween A Thermal Model for the Differentiation of Asteroid 4 Vesta, Based on Radiogenic Heating, Icarus, Vol. 134, p. 187 (1998).
- K. Righter and M. J. Drake A magma ocean on Vesta: Core formation and petrogenesis of eucrites and diogenites, Meteoritics & Planetary Science, Vol. 32, p. 929 (1997).
- M. J. Drake The eucrite/Vesta story, Meteoritics & Planetary Science, Vol. 36, p. 501 (2001).
- R. P. Binzel et al. Geologic Mapping of Vesta from 1994 Hubble Space Telescope Images, Icarus, Vol. 128, p. 95 (1997).
- B. J. Zellner et al. Hubble Space Telescope Images of Asteroid Vesta in 1994, Icarus, Vol. 128, p. 83 (1997).
- M. S. Kelley et al. Quantified mineralogical evidence for a common origin of 1929 Kollaa with 4 Vesta and the HED meteorites, Icarus, Vol. 165, p. 215 (2003).
- Amos, Jonathan 2012. Asteroid Vesta is 'last of a kind' rock. BBC News: Science & environment. 
- Greg Bryant. "Sky & Telescope: See Vesta at Its Brightest!". http://www.skyandtelescope.com/observing/home/7297386.html. Retrieved 2007-5-7.
- Sky & Telescope, Vesta Finder. Retrieved on May 7, 2007.
- Yeomans, Donald K.. "Horizons system". NASA JPL. http://ssd.jpl.nasa.gov/?horizons. Retrieved 2007-3-20. — Horizons can be used to obtain a current ephemeris
- K. Keil, Geological History of Asteroid 4 Vesta: The Smallest Terrestrial Planet in Asteroids III, William Bottke, Alberto Cellino, Paolo Paolicchi, and Richard P. Binzel, (Editors), Univ. of Arizona Press (2002), ISBN 0-8165-2281-2
- Views of the Solar System: Vesta
- HubbleSite: Hubble Maps the Asteroid Vesta
- Encyclopaedia Britannica, Vesta - full article
- HubbleSite: Hubble Reveals Huge Crater on the Surface of the Asteroid Vesta
- HubbleSite: short movie composed from Hubble Space Telescope images from November 1994.
- Adaptive optics views of Vesta from Keck Observatory
- Differentiated interior of Vesta
- Orbital simulation from JPL (Java)
- 4 Vesta images at ESA/Hubble
- Hubble views of Vesta on the Planetary Society Weblog (includes animation)
- Farinella, Paolo (2005). "Houston: Focus on Vesta and the HEDs". Arkansas Center for Space & Planetary Sciences. http://meteoritemag.uark.edu/612.htm. Retrieved 2007-10-25.