Asteroids become darker and redder with age due to space weathering. However evidence suggests most of the color change occurs rapidly, in the first hundred thousands years, limiting the usefulness of spectral measurement for determining the age of asteroids.
Color
Asteroid
Asteroid | Color
Asteroids become darker and redder with age due to space weathering. Composition is calculated from three primary sources: albedo, surface spectrum, and density. It is a  is a torus-shaped region in the Solar System, located roughly between the orbits of the planets Jupiter and Mars, that is occupied by a great many solid, irregularly shaped bodies, of many sizes but much smaller than planets, called asteroids or minor planets. It is occupied by a great many solid, irregularly shaped bodies, of many sizes but much smaller than planets, called asteroids or minor planets. It is occupied by a great many solid, irregularly shaped bodies, of many sizes but much smaller than planets, called asteroids or minor planets.
large objects ( 10 m) in space originating from a region between jupiter and mars
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Asteroid belt
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can you explain its structure?
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"" is an assumed C-type asteroid. It has a typical V–I color index of 0.906 "(see table below)".
(15977) 1998 MA11 | Physical characteristics
appears unusually bright for its size, suggesting it is made of brighter materials than the average asteroid.
2018 CB | Physical characteristics
Figure 1 shows the positions of the Hildas (black) against a background of all known asteroids (gray) up to Jupiter's orbit at January 1, 2005. Each of the Hilda objects moves along its own elliptic orbit. However, at any moment the Hildas together constitute this triangular configuration, and all the orbits together form a predictable ring. Figure 2 illustrates this with the Hildas positions (black) against a background of their orbits (gray). For the majority of these asteroids, their position in orbit may be arbitrary, except for the external parts of the apexes (the objects near aphelion) and the middles of the sides (the objects near perihelion).
Hilda asteroid | Dynamics
" is an assumed, carbonaceous C-type asteroid, while most larger Jupiter trojans are D-types. It has a typical V–I color index of 0.97.
(5119) 1988 RA1 | Physical characteristics
"" is an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a typical V–I color index of 0.95 and a BR color of 1.23 "(also see table below)".
(32496) 2000 WX182 | Physical characteristics
" is an assumed, carbonaceous C-type asteroid. It has a V–I color index of 0.875.
(15502) 1999 NV27 | Physical characteristics
In both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), " is a dark D-type asteroid, the dominant spectral type among the larger Jupiter trojans. It has a typical V–I color index of 0.90.
(5648) 1990 VU1 | Physical characteristics
"" is an assumed, carbonaceous C-type asteroid. It has a high V–I color index of 1.00 "(see table below)".
(20729) 1999 XS143 | Physical characteristics
" is an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a typical V–I color index of 0.99 and a BR-color of 1.15.
(23958) 1998 VD30 | Physical characteristics
" is an assumed C-type asteroid. Its V–I color index of 0.95 is typical for most D-type asteroids, the dominant spectral type among the Jupiter trojans.
(34746) 2001 QE91 | Physical characteristics
" is an assumed C-type asteroid. It has a V–I color index of 0.88.
(12929) 1999 TZ1 | Physical characteristics
" is an assumed C-type asteroid, while the majority of large Jupiter trojans are D-types. It has a typical V–I color index of 0.97.
(15440) 1998 WX4 | Physical characteristics
This object has been characterized as a bright Vestian-like V-type asteroid.
(164121) 2003 YT1 | Physical characteristics
" is an assumed C-type asteroid. Its V–I color index of 0.97 is typical for that of D-type asteroids, the dominant spectral type among the Jupiter trojans.
(21601) 1998 XO89 | Physical characteristics
"" is an assumed stony S-type asteroid. This asteroid is a typical contact binary, with two distinctive lobes on either end that appear to be in contact, giving it a peanut-like shape.
(388188) 2006 DP14 | Physical characteristics
" has a V–I color index of 0.99, typical for most D-type asteroid. It is also an assumed C-type.
(38050) 1998 VR38 | Physical characteristics
" is an assumed C-type asteroid. It has a V–I color index of 0.85, slightly below that seen for most Jovian D-type asteroids "(also seen table below)".
(4715) 1989 TS1 | Physical characteristics
In the SDSS-based taxonomy, "" is dark D-type asteroid, which agrees with the determined spectral type by Pan-STARRS. Its V–I color index of 0.91 is typical for most larger Jupiter trojans "(also see table below)".
(6545) 1986 TR6 | Physical characteristics
The moderately bright R-type asteroid has a surface that strongly absorbs in the olivine and pyroxene spectral region, which give it its very reddish color.
1904 Massevitch | Physical characteristics
Analysis of precovery observations in the visible spectrum between 2002 and 2007 show that it may be amongst the reddest objects in the Solar System, being more than 1.5 magnitudes fainter in the G (green) filtered versus the R (red) filtered images, which may offer some clues about its composition and origin "(also see color indices)". This is expected from a fairly small "orbitally unexcited" cold Classical Kuiper belt object as they are generally mostly red. The cold populations distance does not vary from the Sun very much so their surfaces are older, more irradiated, and covered in tholins. There is a chance it accreted in basically the same orbit it has today.
420356 Praamzius | Physical characteristics
In the SDSS-based taxonomy, " is a dark D-type asteroid. It has also been characterized as a D-type by Pan-STARRS survey. Its V–I color index of 0.98 agrees with that of most Jovian D-type asteroids.
(7641) 1986 TT6 | Physical Characteristics
The orbit of this asteroid is shown in blue when it is above the plane of the orbit of Jupiter, and in magenta when it is below the plane of the orbit of Jupiter.
514107 Kaʻepaokaʻawela | Orbit
The total mass of the system is . For a realistic minimal density of 0.5 g/cm the albedo is >0.17 and the size of the components is <60 km. The "Collaborative Asteroid Lightcurve Link" assumes an albedo of 0.1 and calculates a diameter of 175.20 kilometers based on an absolute magnitude of 6.9. "Mors–Somnus" has an ultra-red spectrum in the visible and near-infrared parts of the spectrum. The colors of two components are indistinguishable from each other. It demonstrates a double-peaked light curve with the period of about 9.28 hours and amplitude of 0.24. This indicates that either primary of secondary has an elongated shape and rotates non-synchronuosly.
341520 Mors–Somnus | Physical properties
The light curve shows a high amplitude, indicative of its elongated shape, measuring 5.0 × 2.0 × 2.1 kilometers, which corresponds to a mean-diameter of 2.5 km. The interior of the asteroid probably has a rubble-pile structure. The asteroid's high thermal inertia indicates the surface is most likely a mix of fine grains and large rocks and boulders. During the asteroid's close approach to Earth in 1994, a radar study of it was conducted by the Deep Space Network at the Goldstone Observatory, California. The resultant images show Geographos to be the most elongated object in the Solar System.
1620 Geographos | Shape and structure
Over thousands of years the angle between the position of the asteroid and its perihelion minus the angle between Jupiter and the asteroid's perihelion tends to oscillate around zero with a period of about 660 years and an amplitude of about 125°, although sometimes this difference slips by a whole 360°. The adjunct diagram shows one complete orbit of asteroid "Kaʻepaokaʻawela" in a frame of reference rotating with Jupiter. The view is from the north looking south onto the Solar System. The dot in the middle is the Sun and the green circle is the orbit of Earth. The black circle shows the size of the orbit of Jupiter but in this frame of reference Jupiter (the red dot) stays almost stationary at the point on the circle directly to the right of the sun.
514107 Kaʻepaokaʻawela | Orbit
The asteroid is characterized as both a carbonaceous C-type and metallic M-type asteroid. The density of the primary was calculated using the orbital elements of the binary system, the primary-to-secondary mass ratio, and estimates of the primary size. The primary has a low density of 1.7 g/cm, which may indicate a "rubble pile" structure containing rocks and voids.
(185851) 2000 DP107 | Physical characteristics
A photometric sequence such as V–R–B–I can be obtained from observations within a few minutes.
Asteroid spectral types | Color indices
" is an assumed C-type asteroid. Its V–I color index of 0.98 is typical for that of most Jovian D-types, the dominant spectral type among the larger Jupiter trojans.
(6090) 1989 DJ | Physical characteristics
" is an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a high V–I color index of 1.090.
(22149) 2000 WD49 | Physical characteristics
has a dark albedo of 0.04, giving it a diameter of about 291 km. Its reflectance spectrum bears striking resemblance to those of some hydrated C-type asteroids, indicating that this object possibly formed in the same environment as the C-type asteroids found today in the outer asteroid belt. Unlike the majority of small objects in the Kuiper belt observed so far, the visible spectrum of has two features, each respectively associated with ferric oxides and phyllosilicates. The presence of a phyllosilicate feature in the spectrum of a minor planet indicates that the rocky component of its composition has been altered by the presence of liquid water at some point since its formation.
(120216) 2004 EW95 | Physical characteristics
It has the longest rotation period of an asteroid more than 150 km in diameter. As a primitive C-type asteroid it is probably composed of carbonaceous material.
120 Lachesis | Introduction
In the Tholen classification, this object is an uncommon Q-type asteroid, that falls into the larger stony S-complex. As of 2018, no rotational lightcurve of this asteroid has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown. It has a brightness variation of 0.69 magnitude, indicative for an elongated, non-spherical shape.
(85182) 1991 AQ | Physical characteristics
The surface of is covered with a sooty substance, making it optically dark with a geometric albedo of 0.06, meaning it absorbs 94% of the light that hits it, which is indicative for a carbonaceous surface of a C-type asteroid. The asteroid is covered with craters and is dark, red, and primitive.
(285263) 1998 QE2 | Surface, albedo and composition
The asteroid is an assumed stony S-type asteroid.
(467336) 2002 LT38 | Physical characteristics
It is expected to be about half the size of Sedna and similar in size to Huya. Its surface is thought to have a pink tinge, resulting from chemical changes produced by the effect of radiation on frozen water, methane, and carbon dioxide. This optical color is consistent with formation in the gas-giant region and not the classical Kuiper belt, which is dominated by ultra-red colored objects.
2012 VP113 | Classification and physical characteristics
"Krethon" is an assumed, carbonaceous C-type asteroid, while most larger Jupiter trojans are D-types. It has a high V–I color index of 1.09 "(see table below)".
5285 Krethon | Physical characteristics
The observations also revealed that the asteroid has an elongated oblate shape, resembling a "clenched fist". Its surface exhibits multiple kilometer scale ridges and concavities.
(162421) 2000 ET70 | Rotation period, pole, and shape
The asteroid has a mass of (5.99 ± 0.60) × 10 kilograms and a mean density of grams per cubic centimeters, which lies approximately in between the density of limestone and concrete/gravel.
25 Phocaea | Mass and density
The Smithsonian Institution, which surveyed the work as part of its "Save Outdoor Sculpture!" program in 1994, suggests the sculpture is made of wire mesh, fiberglass, and resin. It measures approximately x x and is supported by a base of metal pipes, each of which are approximately tall and have a diameter of . Smithsonian considers the work abstract and deemed its condition "treatment needed" the year it was surveyed. It is administered by the University of Oregon.
Brown and Black Asteroid | Description
By comparing the asteroid's perceived brightness and the then computed distance from the Sun they arrived at an absolute visual magnitude of 14.3, which if one assumes Mars-like albedo gives an approximate diameter of 3 to 5 kilometers.
878 Mildred | Physical properties
Alternatively, the site may be of volcanic origin.
Gatun structure | Introduction
Radar observations by the Arecibo Observatory on 14 July 2015, revealed that the asteroid's shape looks like an unshelled walnut with a diameter of 300 by 600 metres. The radiometric observations also agreed with the previously obtained photometric ones and gave a period of 37 minutes.
(436724) 2011 UW158 | Shape
Colour indices are simple measures of the differences in the apparent magnitude of an object seen through blue (B), visible (V), i.e. green-yellow, and red (R) filters. The diagram illustrates known colour indices for all but the biggest objects (in slightly enhanced colour). For reference, two moons: Triton and Phoebe, the centaur Pholus and the planet Mars are plotted "(yellow labels, size not to scale)". Correlations between the colours and the orbital characteristics have been studied, to confirm theories of different origin of the different dynamic classes: While the relatively dimmer bodies, as well as the population as the whole, are reddish (V−I = 0.3–0.6), the bigger objects are often more neutral in colour (infrared index V−I < 0.2).
Trans-Neptunian object | Color indices
It is thought that planetesimals in the asteroid belt evolved much like the rest of the solar nebula until Jupiter neared its current mass, at which point excitation from orbital resonances with Jupiter ejected over 99% of planetesimals in the belt. Simulations and a discontinuity in spin rate and spectral properties suggest that asteroids larger than approximately in diameter accreted during that early era, whereas smaller bodies are fragments from collisions between asteroids during or after the Jovian disruption. Ceres and Vesta grew large enough to melt and differentiate, with heavy metallic elements sinking to the core, leaving rocky minerals in the crust.
Asteroid | Formation
Spectra from the Hale Telescope on 25 October showed red color resembling comet nuclei or Trojans. Higher signal to noise spectra recorded by the William Herschel Telescope later that day showed that the object was featureless, and colored red like Kuiper belt objects. Spectra obtained with the Very Large Telescope the following night showed that behaviour continued into near-infrared wavelengths. Its spectrum is similar to that of D-type asteroids. Oumuamua is rotating around a non-principal axis, a type of movement known as tumbling. This accounts for the various rotation periods reported, such as 8.10 hours (±0.42 hours or ±0.02 hours) by Bannister et al.
ʻOumuamua | Appearance, shape and composition
Mathilde is very dark, with an albedo comparable to fresh asphalt, and is thought to share the same composition as CI1 or CM2 carbonaceous chondrite meteorites, with a surface dominated by phyllosilicate minerals. The asteroid has a number of extremely large craters, with the individual craters being named for coal fields and basins around the world. The two largest craters, Ishikari (29.3 km) and Karoo (33.4 km), are as wide as the asteroid's average radius. The impacts appear to have spalled large volumes off the asteroid, as suggested by the angular edges of the craters. No differences in brightness or colour were visible in the craters and there was no appearance of layering, so the asteroid's interior must be very homogeneous.
253 Mathilde | Characteristics
As of 2018, the asteroid's composition, shape and rotation period remain unknown.
37432 Piszkéstető | Lightcurves
" is an assumed, carbonaceous C-type asteroid. The overall spectral type of members of the Eurybates family is that of a C- and P-type. It has a high V–I color index of 1.01.
(5258) 1989 AU1 | Physical characteristics
This would absorb blue light, creating a reddish hue. Most classical objects display this colour, but scattered objects do not; instead, they present a white or greyish appearance. One explanation is the exposure of whiter subsurface layers by impacts; another is that the scattered objects' greater distance from the Sun creates a composition gradient, analogous to the composition gradient of the terrestrial and gas giant planets. Michael E. Brown, discoverer of the scattered object Eris, suggests that its paler colour could be because, at its current distance from the Sun, its atmosphere of methane is frozen over its entire surface, creating an inches-thick layer of bright white ice.
Scattered disc | Composition
Since its discovery, several other objects were found exhibiting mixed cometary and asteroidal features, such as 133P/Elst–Pizarro, leading to a new class of objects dubbed "active asteroids". In 2018, observations revealed that Phaethon was blue in color, which is an extremely rare occurrence among asteroids. In contrast, most asteroids tend to be grey or red. In 2020, polarimentric study revealed Phaeton has a surface with steep slopes covered by a mix of regolith with larger pebbles. Phaethon's composition fits the notion of its cometary origin; it is classified as a F-type asteroid because it is composed of dark material.
3200 Phaethon | Physical characteristics
Ceres, the only object in the asteroid belt large enough to be a dwarf planet, is about 950 km in diameter, whereas Vesta, Pallas, and Hygiea have mean diameters of less than 600 km. The remaining bodies range down to the size of a dust particle. The asteroid material is so thinly distributed that numerous unmanned spacecraft have traversed it without incident. Nonetheless, collisions between large asteroids do occur, and these can produce an asteroid family whose members have similar orbital characteristics and compositions. Individual asteroids within the asteroid belt are categorized by their spectra, with most falling into three basic groups: carbonaceous (C-type), silicate (S-type), and metal-rich (M-type).
Asteroid belt | Introduction
is an Amor asteroid, because its perihelion is less than 1.3 AU and does not cross Earth's orbit. The asteroid measures approximately 100–240 meters in diameter. Its orbit is within a region of stability where bodies may survive for the age of the Solar System, and hence it may have formed near its current orbit. Between 1900 and 2200 its closest approach to Earth is more than 0.12 AU.
(350462) 1998 KG3 | Description
The asteroid's spectral type is unknown. Based on its albedo "(see below)", it is a stony rather than carbonaceous asteroid.
19139 Apian | Physical characteristics
orbit characterizes it as a classical Kuiper Belt object, or cubewano. Due to its nearly circular orbit and low inclination, it is also in the "cold" population of cubewanos. As a result, it is likely reddish in color.
1999 OJ4 | Orbit and classification
In the SDSS-based taxonomy, "" is a dark D-type asteroid. It has also been characterized as a D-type by Pan-STARRS' survey, while the "Collaborative Asteroid Lightcurve Link" (CALL) assumes it to be a C-type asteroid.
(16070) 1999 RB101 | Physical characteristics
The object is an assumed, common S-type asteroid.
(219774) 2001 YY145 | Physical characteristics
There are indications of material movement along the downslope direction. The density measured by NEAR Shoemaker, 1,300 kg/m³, is less than half that of a typical carbonaceous chondrite; this may indicate that the asteroid is very loosely packed rubble pile. The same is true of several C-type asteroids studied by ground-based telescopes equipped with adaptive optics systems (45 Eugenia, 90 Antiope, 87 Sylvia and 121 Hermione). Up to 50% of the interior volume of Mathilde consists of open space. However, the existence of a 20-km-long scarp may indicate that the asteroid does have some structural strength, so it could contain some large internal components.
253 Mathilde | Characteristics
"Demoleon" is an assumed C-type asteroid, while most larger Jupiter trojans are D-types. It has a low V–I color index of 0.775 "(see table below)".
18493 Demoleon | Physical characteristics
Based on a generic conversion from absolute magnitude, the asteroid measures between 0.6 and 1.4 kilometers in diameter.
(434326) 2004 JG6 | Physical characteristics
Under the SMASS classification taxonomy, this asteroid is listed as a B-type; a group that combines both the Tholen B and F types. The spectrum of this object suggests the presence of magnetite (FeO), which gives it the spectrally-blue coloration that is a characteristic of this SMASS class. The spectrum of this asteroid also displays a band feature near 2.9 μm that indicate the presence of a hydrated mineral. This suggests that the asteroid has undergone significant water-based alteration.
335 Roberta | Introduction
"Pyrrhus" is an assumed C-type asteroid, while most larger Jupiter trojans are D-type asteroids. It has a typical V–I color index of 0.95 "(also see table)".
5283 Pyrrhus | Physical characteristics
is a peanut-shaped contact binary asteroid. It is an assumed stony S-type asteroid.
2014 JO25 | Physical characteristics
, has a diameter approximately , based on an estimated albedo between 0.04 and 0.10 respectively. Astronomer Marc Buie gives a similar estimate of , and the "Johnstons archive" calculated a diameter of 39 km. Based on generic magnitude-to-diameter conversion, the object measures 44 km, for an absolute magnitude of 10.3 and an assumed albedo of 0.07. Hubble observations of show that it is very red in color.
2014 PN70 | Physical characteristics
As of 2017, the asteroid's composition, shape and rotation period remain unknown.
39382 Opportunity | Lightcurves
In the SDSS-based taxonomy, "Askalaphus" is a D-type asteroid. It has also been characterized as a D-type by Pan-STARRS' survey. Its V–I color index of 0.94, is typical for most larger Jupiter trojans "(see table below)".
4946 Askalaphus | Physical characteristics
According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, measures 1.218 kilometers in diameter and its surface has an albedo of 0.157. The asteroid's composition and shape, as well as its rotation period remain unknown. It has an absolute magnitude of 17.2.
(394130) 2006 HY51 | Physical characteristics
" is an assumed, carbonaceous C-type asteroid. Nesvorný does not give an overall spectral type for this unnamed family, but derives an albedo of 0.06 "(see below)", which is also typical for carbonaceous C-types.
(9799) 1996 RJ | Physical characteristics
" has been characterized as a common, stony S-type asteroid. In the SMASS taxonomy, it is an Sk-subtype, that transitions between the S and K-type asteroids. The body's color indices of 0.690 (B–V), 0.500 (V–R) and 0.840 (V–I) were also determined.
(5407) 1992 AX | Physical characteristics
Asteroids become darker and redder with age due to space weathering. However evidence suggests most of the color change occurs rapidly, in the first hundred thousands years, limiting the usefulness of spectral measurement for determining the age of asteroids.
Asteroid | Color
Asteroids except for the largest, Ceres, are classified as small Solar System bodies and are composed mainly of refractory rocky and metallic minerals, with some ice. They range from a few metres to hundreds of kilometres in size. Asteroids smaller than one meter are usually called meteoroids and micrometeoroids (grain-sized), depending on different, somewhat arbitrary definitions. The asteroid belt occupies the orbit between Mars and Jupiter, between from the Sun. It is thought to be remnants from the Solar System's formation that failed to coalesce because of the gravitational interference of Jupiter. The asteroid belt contains tens of thousands, possibly millions, of objects over one kilometre in diameter.
Solar System | Asteroid belt
Sylvia is very dark in color and probably has a very primitive composition. The discovery of its moons made possible an accurate measurement of the asteroid's mass and density. Its density was found to be very low (around 1.2 times the density of water), indicating that the asteroid is porous to very porous; from 25% to as much as 60% of it may be empty space, depending on the details of its composition. However, the mineralogy of the X-type asteroids is not known well enough to constrain this further. Either way, this suggests a loose rubble pile structure. Sylvia is also a fairly fast rotator, turning about its axis every 5.18 hours (giving an equatorial rotation velocity of about 230 km/h or 145 mph).
87 Sylvia | Physical characteristics
' has a very reddish color (RR), indicative of a non-carbonaceous composition rich in tholins and methane. According to the "Johnston's archive", the object only measures 93 kilometers in diameter based on an absolute magnitude of 8.4, and an assumed albedo of 0.09 for the body's surface. Since it is far too small for being considered a dwarf planet candidate, it is not listed at Michael Brown website. As of 2018, no rotational lightcurve of ' has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.
1999 TR11 | Physical characteristics
The asteroid belt is located between Mars and Jupiter. It is made of thousands of rocky planetesimals from to a few meters across. These are thought to be debris of the formation of the Solar System that could not form a planet due to Jupiter's gravity. When asteroids collide they produce small fragments that occasionally fall on Earth. These rocks are called meteorites and provide information about the primordial solar nebula. Most of these fragments have the size of sand grains. They burn up in the Earth's atmosphere, causing them to glow like meteors.
Geology of solar terrestrial planets | Asteroid belt
Based on the asteroids brightness and assumed proximity to Earth, the asteroid was originally estimated to be only 30 meters in diameter.
(444004) 2004 AS1 | Description
Coronagraphic optical observations with the Hubble Space Telescope show complex spiral patterns in the circumstellar disk. The causes of these structures remain uncertain. The disk colors are similar to those derived for Kuiper Belt objects, suggesting that the same weathering processes are at work in HD 100546. The disk is fairly flat, consistent with an advanced evolutionary state. Spectroscopic analysis of mid-IR data taken from OSCIR on the 4 m Blanco Telescope at Cerro Tololo Inter-American Observatory indicates the presence of a small particles (10–18 μm) containing silicates. The material is found at distances out to 17 AU away from the star and has a temperature of approximately 227 K.
HD 100546 | Protoplanetary material
Yellow light is reflected directly from the centres of the pits; blue light is reflected twice by the sides of the pits. The combination appears green, but can be seen as an array of yellow spots surrounded by blue circles under a microscope. Crystal fibres, formed of hexagonal arrays of hollow nanofibres, create the bright iridescent colours of the bristles of "Aphrodita", the sea mouse, a non-wormlike genus of marine annelids. The colours are aposematic, warning predators not to attack. The chitin walls of the hollow bristles form a hexagonal honeycomb-shaped photonic crystal; the hexagonal holes are 0.51 μm apart.
Structural coloration | Fixed structures
Based upon its spectral characteristics, this object is classified as a K-type asteroid. The orbital properties show it to be a member of the extensive Eos asteroid family, which is named after it. The spectral properties of the asteroid suggest it may have come from a partially differentiated parent body.
221 Eos | Introduction
" is an assumed, carbonaceous C-type asteroid.
(3708) 1974 FV1 | Physical characteristics
A 2016 study found to have a comet-like albedo of 2.9% (darker than any other known ejected centaur) and a color typical of D-type asteroids. It is unknown if it is a so-called "super comet" or an extinct comet, considering its large distance from the Sun. It was also determined that has a diameter of kilometers, larger than initially believed. A light curve analysis found it to have a rotation period of hours, typical of asteroids its size. No significant satellites were detected. It was also found that is on an extremely unstable orbit, with a ~64% chance of being ejected from the Solar system in 1 million years, and a ~25% chance of being ejected in the next 500,000 years, as well as a 4.2% chance of its orbit venturing into the neighborhood of Earth.
2013 AZ60 | Physical characteristics and orbit
Each SPHERES satellite resembles an 18-sided polyhedron. The aluminum structure of the satellite is enclosed in a semi-transparent plastic shell. The shell is red, blue, orange or black in color, to help with easy identification. The three satellites in the International Space Station are red, blue and orange. Each unit has a maximum diameter of 22.9 cm and has a mass of 4.16 kg including the consumables.
SPHERES | Structure and physical characteristics
An asteroid spectral type is assigned to asteroids based on their emission spectrum, color, and sometimes albedo. These types are thought to correspond to an asteroid's surface composition. For small bodies that are not internally differentiated, the surface and internal compositions are presumably similar, while large bodies such as Ceres and Vesta are known to have internal structure. Over the years, there has been a number of surveys that resulted in a set of different taxonomic systems such as the Tholen, SMASS and Bus–DeMeo classification.
Asteroid spectral types | Introduction
has been characterized as a dark D-type asteroid on images taken by the Sloan Digital Sky Survey. Conversely, Pan-STARRS photometric survey determined a much brighter S-type.
(7025) 1993 QA | Physical characteristics
On 5 March 2001, " made a close approach to Earth at a distance of . It was studied by radar at the Goldstone and Arecibo observatories from March 3 to 7, 2001. The studies showed that the asteroid has a mean diameter of 1.1 km, assuming that ' is a retrograde rotator. Optical lightcurve analysis by Lenka Sarounova and Petr Pravec shows that its rotation period is hours. Due to its short rotation period and high radar albedo, ' is thought to be fairly dense (more than 3.5 g/cm, assuming that it has no internal strength) and likely composed of nickel–iron.
(29075) 1950 DA | Observations
The carbonaceous asteroid has been characterized as a dark and reddish P-type asteroid by the Wide-field Infrared Survey Explorer (WISE), and as an X-type asteroid by Pan-STARRS photometric survey.
1042 Amazone | Physical characteristics
The asteroid has been characterized as an L- and S-type asteroid by Pan-STARRS large-scale survey.
3267 Glo | Physical characteristics
has been characterized as an uncommon Q-type asteroid, that fall into the larger stony S-complex.
(163243) 2002 FB3 | Physical characteristics
"Amphilochos" is an assumed C-type asteroid, while the majority of larger Jupiter trojans are D-types. It has an untypically low V–I color index of 0.77 "(see table below)".
5244 Amphilochos | Physical characteristics
"Cloanthus" is an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the remainder being mostly C and P-type asteroids. It has a V–I color index of 0.890 and a BR color of 1.21 "(also see table below)".
5511 Cloanthus | Physical characteristics
The Minor Planet Center estimates a diameter of , concurring with other estimates of . As of 2018, no rotational lightcurve of this object has been obtained from photometric observations. The asteroids's rotation period, pole and shape remain unknown.
2018 BF3 | Physical characteristics
"Ilioneus" is an assumed C-type asteroid. Its V–I color index of 0.96 is typical for most D-type asteroids, the dominant spectral type among the Jupiter trojans.
5130 Ilioneus | Physical characteristics
" is an assumed C-type asteroid.
(457175) 2008 GO98 | Physical characteristics
The reason for this variation has to do with the shape of the asteroid.
232 Russia | Introduction
"Iphidamas" is an assumed, carbonaceous C-type asteroid. It has a high V–I color index of 1.03 "(see table below)".
4791 Iphidamas | Physical characteristics
"Sthenelos" is an assumed, carbonaceous C-type asteroid, while most larger Jupiter trojans are D-type asteroids. It has a high V–I color index of 1.07.
3794 Sthenelos | Physical characteristics
The curve is asymmetrical with four uneven minima and maxima. Occultation data from October 9, 2006 using 15 chords shows the asteroid is about 130 km in diameter.
200 Dynamene | Introduction
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures () kilometers in diameter and its surface has an albedo of () based on an absolute magnitude of 18.9. Radar observations at Goldstone suggest that the object is elongated and irregular in shape, with its long axis measuring at least . Lance Benner suspects it the be a contact binary, composed of two merged objects forming a single asteroid with a lobed shape. Photometric observations by astronomers with the "Mission Accessible Near-Earth Objects Survey" (MANOS) and subsequent evaluation by Brian Warners "Collaborative Asteroid Lightcurve Link", determined that has a rotation period of at least 16 hours.
2014 HQ124 | Physical characteristics
Due to its higher than usual brightness variation, this Jovian asteroid is likely to have a non-spherical shape.
5264 Telephus | Rotation period
This is consistent with the asteroid dimensions computed through other means. Based upon a light curve that was generated from photometric observations of this asteroid at Pulkovo Observatory, it has a rotation period of 12.834 ± 0.001 hours and varies in brightness by 0.15 ± 0.01 in magnitude.
38 Leda | Introduction
is an assumed, stony S-type asteroid.
(90075) 2002 VU94 | Physical characteristics
, provisionally known as , is a resonant trans-Neptunian object in the Kuiper belt located in the outermost regions of the Solar System. It measures approximately 291 kilometers in diameter. It has more carbon than typical of KBOs, and the first to be confirmed as having this composition in this region of space. It is thought that it had originated closer to the Sun, maybe even the main asteroid belt.
(120216) 2004 EW95 | Introduction