433 Eros

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433 Eros
Eros - PIA02923 (color).jpg
Eros [1]
Discovery [2]
Discovered byG. Witt
Discovery siteBerlin Urania Obs.
Discovery date13 August 1898
MPC designation(433) Eros
Named after
Eros (Greek mythology)[3]
1898 DQ · 1956 PC
NEO · Amor (I)[2]
Orbital characteristics[2]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc53.89 yr (19,683 days)
Aphelion1.7825 AU
Perihelion1.1334 AU
1.4579 AU
1.76 yr (643 days)
0° 33m 35.64s / day
Earth MOID0.1505 AU · 58.6 LD
Physical characteristics
Dimensions16.84±0.06 km (mean diameter)[2][4]
34.4 × 11.2 × 11.2 km[2][5]
Mass(6.687±0.003)×1015 kg[4]
Mean density
2.67±0.03 g/cm³[2][4]
5.270 h[2]
S (Tholen), S (SMASS)[2]
B–V = 0.921[2]
U–B = 0.531[2]

433 Eros (/ˈɪərɒs/ EER-os), provisional designation 1898 DQ, is a stony and elongated asteroid of the Amor group and the first discovered and second-largest near-Earth object with a mean-diameter of approximately 16.8 kilometers. Visited by the NEAR Shoemaker space probe in 1998, it became the first asteroid ever studied from orbit.

The eccentric asteroid was discovered by German astronomer Carl Gustav Witt at the Berlin Urania Observatory on 13 August 1898, and later named after Eros, a god from Greek mythology.[3]



Eros was discovered on 13 August 1898, by Carl Gustav Witt at Berlin Urania Observatory and Auguste Charlois at Nice Observatory.[7] Witt was taking a 2-hour exposure of Beta Aquarii to secure astrometric positions of asteroid 185 Eunike.[8]

Later studies

During the opposition of 1900–1901, a worldwide program was launched to make parallax measurements of Eros to determine the solar parallax (or distance to the Sun), with the results published in 1910 by Arthur Hinks of Cambridge.[9] A similar program was then carried out, during a closer approach, in 1930–1931 by Harold Spencer Jones.[10] The value obtained by this program was considered definitive until 1968, when radar and dynamical parallax methods became more important.

Eros was the first asteroid detected by the Arecibo Observatory's radar system.[11][12]

Eros was one of the first asteroids visited by a spacecraft, the first one orbited, and the first one soft-landed on. NASA spacecraft NEAR Shoemaker entered orbit around Eros in 2000, and landed in 2001.


Eros is a Mars-crosser asteroid, the first known to come within the orbit of Mars. Objects in such an orbit can remain there for only a few hundred million years before the orbit is perturbed by gravitational interactions. Dynamical integrations suggest that Eros may evolve into an Earth-crosser within as short an interval as two million years, and has a roughly 50% chance of doing so over a time scale of 108–109 years.[13] It is a potential Earth impactor,[13] about five times larger than the impactor that created Chicxulub crater and led to the extinction of the dinosaurs.[14]


Eros is named after the Greek god of love, Erōs. It is pronounced /ˈɪərɒs/ EER-os or sometimes /ˈɛrɒs/ ERR-os. The rarely used adjectival form of the name is Erotian /ɪˈrʃən/. Eros is also the first masculine name for an asteroid.[15]

NEAR Shoemaker

Animation of NEAR Shoemaker trajectory from May 31, 1996 to February 12, 2001.
Template:Font color; Template:Font color; Template:Font color;   253 Mathilde ; Template:Font color
Animation of NEAR Shoemaker's trajectory around 433 Eros from April 1, 2000 to February 12, 2001
   NEAR Shoemaker ·   433 Eros

The NEAR Shoemaker probe visited Eros twice, first with a 1998 flyby, and then by orbiting it in 2000 when it extensively photographed its surface. On February 12, 2001, at the end of its mission, it landed on the asteroid's surface using its maneuvering jets.

Physical characteristics

Surface gravity depends on the distance from a spot on the surface to the center of a body's mass. Eros's surface gravity varies greatly because Eros is not a sphere but an elongated peanut-shaped (or potato- or shoe-shaped) object. The daytime temperature on Eros can reach about 100 °C (373 K) at perihelion. Nighttime measurements fall near −150 °C (123 K). Eros's density is 2.67 g/cm3, about the same as the density of Earth's crust. It rotates once every 5.27 hours.

NEAR scientists have found that most of the larger rocks strewn across Eros were ejected from a single crater in an impact approximately 1 billion years ago.[16] (The crater involved was proposed to be named "Shoemaker", but is not recognized as such by the International Astronomical Union (IAU), and has been formally designated Charlois Regio.) This event may also be responsible for the 40 percent of the Erotian surface that is devoid of craters smaller than 0.5 kilometers across. It was originally thought that the debris thrown up by the collision filled in the smaller craters. An analysis of crater densities over the surface indicates that the areas with lower crater density are within 9 kilometers of the impact point. Some of the lower density areas were found on the opposite side of the asteroid but still within 9 kilometers.[17]

It is theorized that seismic shockwaves propagated through the asteroid, shaking smaller craters into rubble. Since Eros is irregularly shaped, parts of the surface antipodal to the point of impact can be within 9 kilometres of the impact point (measured in a straight line through the asteroid) even though some intervening parts of the surface are more than 9 kilometres away in straight-line distance. A suitable analogy would be the distance from the top centre of a bun to the bottom centre as compared to the distance from the top centre to a point on the bun's circumference: top-to-bottom is a longer distance than top-to-periphery when measured along the surface but shorter than it in direct straight-line terms.[17]

Compression from the same impact is believed to have created the thrust fault Hinks Dorsum.[18]

Data from the Near Earth Asteroid Rendezvous spacecraft collected on Eros in December 1998 suggests that it could contain 20,000 billion kilograms of aluminum and similar amounts of metals that are rare on Earth, such as gold and platinum.[19]

Visibility from Earth

Path in sky during opposition 2011/2012

On January 31, 2012, Eros passed Earth at 0.17867 AU (26,729,000 km; 16,608,000 mi),[20][21] about 70 times the distance to the Moon, with a visual magnitude of +8.1.[22] During rare oppositions, every 81 years, such as in 1975 and 2056, Eros can reach a magnitude of +7.0,[6] which is brighter than Neptune and brighter than any main-belt asteroid except 1 Ceres, 4 Vesta and, rarely, 2 Pallas and 7 Iris. Under this condition, the asteroid actually appears to stop, but unlike the normal condition for a body in heliocentric conjunction with Earth, its retrograde motion is very small. For example, in January and February 2137, it moves retrograde only 34 minutes in right ascension.[2]


See also



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  4. 4.0 4.1 4.2 Yeomans, D. K.; Antreasian, P. G.; Barriot, J.-P.; Chesley, S. R.; Dunham, D. W.; Farquhar, R. W. et al. (September 2000). "Radio Science Results During the NEAR-Shoemaker Spacecraft Rendezvous with Eros". Science 289 (5487): 2085–2088. Bibcode 2000Sci...289.2085Y. doi:10.1126/science.289.5487.2085. ISSN 0036-8075. PMID 11000104. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2000Sci...289.2085Y. Retrieved 16 August 2017.
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  7. Scholl, Hans; Schmadel, Lutz D. (2002). "Discovery Circumstances of the First Near-Earth Asteroid (433) Eros". Acta Historica Astronomiae 15: 210–220. Bibcode 2002AcHA...15..210S.
  8. Yeomans, Donald K.; Asteroid 433 Eros: The Target Body of the NEAR Mission Archived 2007-09-28 at the Wayback Machine., Jet Propulsion Laboratory/California Institute of Technology.
  9. Hinks, Arthur R. (1909). "Solar Parallax Papers No. 7: The General Solution from the Photographic Right Ascensions of Eros, at the Opposition of 1900". Monthly Notices of the Royal Astronomical Society 69 (7): 544–67. Bibcode 1909MNRAS..69..544H. doi:10.1093/mnras/69.7.544.
  10. Jones, H. Spencer (1941). "The Solar Parallax and the Mass of the Moon from Observations of Eros at the Opposition of 1931". Mem. Roy. Astron. Soc. 66: 11–66.
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  13. 13.0 13.1 Michel, Patrick; Farinella, Paolo; Froeschlé, Christiane (1996-04-25). "The orbital evolution of the asteroid Eros and implications for collision with the Earth". Nature 380 (6576): 689–691. Bibcode 1996Natur.380..689M. doi:10.1038/380689a0. http://www.nature.com/nature/journal/v380/n6576/abs/380689a0.html. Retrieved 2011-02-12.
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  16. Thomas, P. C.; Veverka, J.; Robinson, M. S.; Murchie, S. (2001-09-27). "Shoemaker crater as the source of most ejecta blocks on the asteroid 433 Eros". Nature 413 (6854): 394–396. Bibcode 2001Natur.413..394T. doi:10.1038/35096513. ISSN 0028-0836. PMID 11574880.
  17. 17.0 17.1 Thomas, P. C.; Robinson, M. S. (2005-07-21). "Seismic resurfacing by a single impact on the asteroid 433 Eros". Nature 436 (7049): 366–369. Bibcode 2005Natur.436..366T. doi:10.1038/nature03855. PMID 16034412.
  18. Watters, T. R.; Thomas, P. C.; Robinson, M. S. (2011). "Thrust faults and the near-surface strength of asteroid 433 Eros". Geophysical Research Letters 38 (2). Bibcode 2011GeoRL..38.2202W. doi:10.1029/2010GL045302. ISSN 0094-8276.
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External links

Further reading

  • Clark, C. S.; Clark, P. E (March 13–17, 2006). "Using Boundary-based Mapping Projections to Reveal Patterns in Depositional and Erosional Features on 433 Eros". 37th Annual Lunar and Planetary Science Conference 37: 1189. Bibcode 2006LPI....37.1189C.
  • Riner, M. A. (November 2008). "Global survey of color variations on 433 Eros: Implications for regolith processes and asteroid environments". Icarus 198 (1): 67–76. Bibcode 2008Icar..198...67R. doi:10.1016/j.icarus.2008.07.007.

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