This article is about the asteroid. For the dwarf planet with a similar name, see Eris (dwarf planet).
433 Eros
Eros – composite image of the north polar region, with the craters Psyche above and Himeros below. The long ridge Hinks Dorsum, believed to be a thrust fault, can be seen snaking diagonally between them. The smaller crater in the foreground is Narcissus. Watters, (2011)
Eros is named after the Greek god of love, Erōs. It was the first minor planet to be given a male name;[3] the break with earlier tradition was made because it was the first near-Earth asteroid discovered.
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.
Mars-crosser
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 system modeling suggests 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.[18] It is a potential Earth impactor,[18] about five times larger than the impactor that created Chicxulub crater and led to the extinction of the non-avian dinosaurs.[a]
NEAR Shoemaker survey and landing
The NEAR Shoemaker probe visited Eros twice, first with a brief flyby in 1998, and then by orbiting it in 2000, when it extensively photographed its surface. On 12 February 2001, at the end of its mission, it landed on the asteroid's surface using its maneuvering jets.
This was the first time a Near Earth asteroid was closely visited by a spacecraft.[19]
Animation of NEAR Shoemaker trajectory from 19 February 1996 to 12 February 2001.
Animation of NEAR Shoemaker's trajectory around 433 Eros from 1 April 2000 to 12 February 2001. NEAR Shoemaker· 433 Eros
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 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.
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.[20] (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.[21]
It is thought that seismic shockwaves propagate 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.[21]
Compression from the same impact is believed to have created the thrust fault Hinks Dorsum.[22]
A phenomenon named dust ponds were discovered in the asteroid in October 2000. Dust ponds are a phenomenon where pockets of dust are seen in airless celestial bodies. These are smooth deposits of dust accumulated in depressions on the surface of the body (like craters), contrasting from the rocky terrain around them. [23] They typically have different color and albedo compared to the surrounding areas. The asteroid contains lots of large craters more than 200 m in diameter. Their number is near to the saturation point of these craters. But craters smaller than that are relatively low. Suggesting that some process of erasure has covered them up. The floors of some craters are covered with smooth and flat areas (less than 10° slope). Such dust ponds are characterized by slightly bluer colour compared to the surrounding terrain. 334 of such ponds are identified, with a diameter of 10m. 255 of these are larger than 30m, and 231 (or 91%) are found within 30° from equator.
Data from the Near Earth Asteroid Rendezvous spacecraft collected on Eros in December 1998 suggests that it could contain 20 billion tonnes of aluminum and similar amounts of metals that are rare on Earth, such as gold and platinum.[24]
Visibility from Earth
Path in sky during opposition 2011/2012
On 31 January 2012, Eros passed Earth at 0.17867 AU (26,729,000 km; 16,608,000 mi),[25][26] about 70 times the distance to the Moon, with a visual magnitude of +8.1.[27] During rare oppositions, every 81 years, such as in 1975 and 2056, Eros can reach a magnitude of +7.0,[7] 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.[1]
In popular culture
In the novel and television series The Expanse, a catastrophic science experiment is unleashed on a civilian population living within tunnels cut through Eros. This so-called "Eros Incident" ends with the asteroid mysteriously breaking its usual orbit and crashing into Venus.[28]
It makes an appearance in the novel (and its film adaptation) Ender's Game by Orson Scott Card, serving as a base for humanity and the location of Command School after having been captured from the invading aliens (the Formics) prior to the initial novel who had used the asteroid as their forward operating base in their previous invasion.[29]
In the Space Angel episode 'Visitors from Outer Space' (title text not quite matching narration), Scott McCloud and his crew are forced to destroy Eros by deflecting it into the Sun, after it becomes a hazard to spacecraft navigation.[30]
^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.
^Perrine, Charles D. (1910). Determination of the solar parallax from photographs of Eros made with the Crossley reflector of the Lick Observatory, University of California (Report). Washington, DC: Carnegie Institution of Washington. pp. 1–104.
^ ab
Michel, Patrick; Farinella, Paolo; Froeschlé, Christiane (25 April 1996). "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. S2CID4354612.
Clark, C.S.; Clark, P.E. (13–17 March 2006). Using boundary-based mapping projections to reveal patterns in depositional and erosional features on 433 Eros. 37th Annual Lunar and Planetary Science Conference. League City, Texas. p. 1189. Bibcode:2006LPI....37.1189C. Abstract no.1189.
.jpg)
.svg){kind=small}
