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Just in our Solar System alone there are billions of moving bodies beside the planets and their satellites. One class consists of rocky bodies of varying compositions: carbonaceous chondrites, chondrites and metallic iron objects (similar to the meteorites that fall on Earth). Most of the meteorites come from the asteroids whose sizes range from less than a kilometer to hundreds of kilometers. Nearly all have irregular shapes. Most lie as a swarm of unconnected bodies in the Main Asteroid Belt between Mars and Jupiter. Others occupy different orbital regions, some of which periodically cross Earth’s orbital path. The other class consists of comets which are relatively small "dirty ice balls" or a nucleus of ice and rock. As those with certain orbits approach the Sun, the solar wind and other forces cause them to ablate, developing a small local atmosphere or coma and eventually a tail of particles which along with the coma glow brightly from sunlight. Comets have a wide range of orbits, some near the solar ecliptic, others at high angles, but all still under the influence of the Sun’s gravity. The Oort Cloud and the Kuiper Belt are two sources that lie well beyond the orbit of Neptune. Long period comets come from great distances such as these sources or elsewhere; short period comets tend to have orbits much closer to the distances defined by planet paths. Both comets and asteroids occasionally strike the Earth. Programs to detect possible bodies that could threaten Earth are now activated.


Asteroids and Comets

A helpful overview of spacecraft visits to asteroids and comets is found during a JPL lecture series webcast. Access this at von Karman lectures, choosing the topic "Comets and Asteroids", June 20, 2002.

A very large number of small (less than 1500 km maximum dimension) bodies composed of rock/dust, ice and condensed gases orbit around the Sun as asteroids and comets. The asteroids are composed mainly of rock, with some ice, and are detectable by solar light reflected from their low albedo surfaces. The comets generally are dominantly ice with some rocky material that are visible because solar light reflects from an envelope of gases collected around an ice/rock nucleus.

Three good overviews of asteroids and comets are found at these sites: (1), (2), and (3).

About 7000 asteroids have been discovered as individuals so far (some astronomers have estimated a total of at least 400,000 larger than 1 km exist within the solar system; the total number, including small ones is likely well in excess of a million). More being found each year owing to a stepped-up search program (see below). The number of known comets is smaller.

Interest has always been high regarding comets, balls of ice and rock, because of their spectacular appearances (glowing "stars" with tails); they are well represented in mythologies and astrologers portents. In the 20th Century, the asteroids, solid fragments of varying size that orbit in several regions of the inner solar system, have had dramatic increases in interest, in part because they are the more frequent bodies that have collided with the Earth and the Moon, and most other larger solar bodies, producing impact craters which on our planet could have (and have had) diastrous consequences - castastrophic in terms of effect on life - of magnitudes only now being properly appreciated. We will start this review with the nature and distribution of asteroids.

About 7000 asteroids have been discovered as individuals so far (some astronomers have estimated a total of at least 400,000 larger than 1 km exist within the solar system; the total number, including small ones is likely well in excess of a million). More being found each year owing to a stepped-up search program (see below). The number of known comets is smaller.

Tens of thousands of asteroids occupy the Main Belt, an interval of mean distance 2.4 A.U., between Mars and Jupiter. Telescopic observations have indicated that about 75% of the asteroids have very low albedos, which is consistent with compositions that are similar to carbonaceous chondrite meteorites, postulated as the most primitive solar system material. Other (about 17%) asteroid groups occur in different locations, such as the Apollo belt (Earth-crossing) and Trojan belt (Jupiter-crossing). Many of the Trojan's are darker and redder. As they orbit the Sun, they also rotate, some with periods of a few days to a week or so and others in a matter of hours ("tumble").

Comets are easier to detect than smaller asteroids. They have higher albedos, and thus are brighter, and as they enter the region of the Solar System within the outer planets they develop luminous tails. Asteroids, on the other hand, present greater difficulties in finding them and determining their orbits. Most asteroids have such low albedos that they don't begin to reflect enough sunlight until relatively close to Earth. Only the larger ones in the Main Asteroid Belt are fairly easy to spot and measure. To illustrate detection techniques, let us describe how the Near Earth Asteroids (NEA), the Apollo belt, are found and monitored to determine their size and orbits.

Optical telescopes, with mirrors around a meter in diameter, are the instruments most commonly used. A portion of the sky (usually around 1 to 10 Moon diameters in width) is viewed over a short time interval (minutes to a few hours). Successive views are recorded on film or electronically using CCDs. Stars and galaxies will retain their fixed positions relative to each other during the interval. An asteroid will look much like these fixed distant stellar/galactic bodies if it is close enough to "shine". But being very close with respect to the distant background, it can move a measurable distance in that time. Consider this trio of telescope photos:

Telephoto containing the asteroid Ryokan.

In the left and center photos, all the starlike objects appear to be in the same fixed positions. But one such body, in right center, actually moves to a slightly new position, towards the upper left, in the middle photo. When the two photos are superimposed, as shown in the right image, two "stars" appear instead of one. The left "star" in the pair is just the same body that has moved in this time interval (30 minutes). This is explained by assuming the body is so close to the Earth that its motion is discernible over short time periods. The presumption is that it is an asteroid. Working with that idea, the actual distance of the object from Earth is determined by parallax (using two telescopes). Once that has been calculated, the size of the body can be estimated (taking its albedo into account) and its velocity is likewise determined from the distance/time relation. Repeated observations allow its orbital parameters to be specified.

The Earth-crossing asteroids all are less than 10 km in maximum dimension. From actual counts, plus extrapolations, the number of Earth-crossing asteroids greater than 1 km in diameter is now placed between 700 and 1000; a collision with Earth for one of that size is estimated to be around 1 per 1-2 million years and for a 10 km asteroid once every 100 million years. The majority of all asteroids have irregular shapes.

Among the Main Belt asteroids the biggest is Ceres (933 km [583 miles]); second in size is Pallas (530 km [331 miles) and Vesta is slightly smaller; these all reside in the Main Belt. The larger asteroids tend to approach spherical in shape. At least some of these have melted and differentiated, so that they have developed iron-rich cores, and possibly a mantle with dispersed metallic iron (the pallasite meteorites may derive from this). One school of planetologists considers these to be "small planets".

Asteroids have been imaged by conventional telescopes, by radar, and by passing or orbiting space probes. This first image shows that ground telescopes do not normally produce good images, even of the larger asteroids, such as Ceres. Compare this to the image made by the Hubble Space Telescope.

The asteroid Ceres as imaged from Earth by an optical telescope.

HST view of Ceres; the nature of the large white spot is presently unknown.

Vesta, at 525 km (325 miles) in long dimension, has been imaged by the Hubble Space Telescope, as seen here:

Vesta seen by HST (left top), reconstructed into sharper detail by a computer program (right top), and displayed as approximations of elevation difference (bottom).

Although not shown clearly, there appears to be a large impact crater with a central peak on Vesta. Spectral analysis of light from Vesta produces values that are very close to the mineral group of pyroxenes. In 1960, a meteorite was found in Western Australia that is entirely pyroxenite (making this a rare type). Many asteroid specialists believe this came from Vesta; if so, it is our first sample of an asteroid that we can analyze.

A pyroxene-rich meteorite which may have come from Vesta.

Both ground telescope and even HST images of small objects such as asteroids are blurry. Thus, to effectively image in detail an asteroid a space probe needs to visit its vicinity. The Galileo spacecraft was programmed to transit close to two asteroids. It passed the first, Gaspra, in 1991. This asteroid, 19 x 12 x 11 km (~12 x 7.5 x 7 mi) in size, consists of iron-nickel and iron-magnesium-rich silicates. This is how it appears in color:

Galileo image of the asteroid Gaspra, 1991.

Galileo approached and imaged the second asteroid, Ida, on August 28, 1993, as shown here (at about 33 m [108 ft]) resolution:

Galileo image of the asteroid Ida, August 28 1993.

This asteroid, about 58 km x 23 km (36 mi x 14 mi) in dimensions, is chondritic and, like Ida, pockmarked with craters. Totally unexpected was the presence of a small orbiting body, about 1.5 km by 1.2 km (0.93 mi x 0.75 mi), named Dactyl–making this pair the first known binary asteroids. Close-up, Dactyl has a small crater, making it look a bit like Saturn's Mimas in miniature:

Galileo image of Dactyl, a small body unexpectedly found orbiting the asteroid Ida.

The first visit exclusively to the asteroid belt has been made by NEAR, for Near Earth Asteroid Rendezvous mission, launched in June 1997 to reach the large asteroid Eros in January, 1999. (After launch, the spacecraft had the name Shoemaker added to it, in memory of the Dean of Astrogeologists, Dr. Eugene M. Shoemaker [see bottom of next page]). Enroute NEAR-Shoemaker took a close look at Mathilde (59 x 47 km) on June 22, 1999 as seen here:

NEAR image of the asteroid Mathilde.

Mathilde has one of the lowest albedos, less than 4%, of any asteroidal object. It also has a low density, 1.4 g/cc, indicating that much of its interior is either ice and/or voids - thus it has been described as a "fluffy" ball. It solid component has probably a carbonaceous chondrite composition.

In 2000, NEAR has successfully orbited Eros and has takbe data on its composition. Below is a view of Eros, whose dimensions of 33 x 13 x 13 km give it a peanut-like shape. Eros is rapidly rotating, as evident from the different positions over a short time span on a December 1998 date.

The large asteroid Eros, as imaged by the NEAR mission camera.

NEAR has operated successfully around EROS for several years, taking thousands of images at various resolutions from different orbital heights. This next image is one of the best, taken in a false color mode in which a green and two NIR bands are used.

NEAR image of EROS.

Here are three views of parts of EROS:

Three views of EROS' surface, made by NEAR-Shoemaker cameras.

Here is a close-up (resolution: just a few meters) of a crater on Eros:

Close-up of a crater on Eros, taken with the NEAR camera.

After completion of the NEAR mission, the mappers gave names to the major features on a flattened mosaic of its surface, as follows:

Image mosaic of Eros, with the named principal features.

NEAR Shoemaker made a close approach to EROS, reaching an altitude just 6 km (4 miles) above its surface, on October 27, 2000. Here is part of a mosaic of images made during that pass. This view shows a crater and rock debris as small as 1 meter across:

Surface of EROS taken 6 km above the surface, showing rocks 10 m down to about 1 m in long dimension.

In early 2001, it was evident that the spacecraft's fuel was nearly depleted. The NEAR scientists and managers pondered how to finish the mission and decided on a bold course - to land the spacecraft on EROS's surface. The asteroid was 196,000 miles from Earth; if successfull this would be the farthest any manmade object had set down on a solid body in the Solar System. Good operational maneuvering and some real luck were essential to the endeavor. Here is the target area chosen:

Image of EROS with a selected touchdown point for the NEAR spacecraft.

The landing attempt began in the afternoon (EST) of February 12. Five burns (fuel blasts) were involved over a 50 minute interval, each slowing the spacecraft and thus causing it to drop ever closer to the surface. The last burn dropped the descent speed to 6 km/hr (4 mph). All the while, images were taken and radioed to Earth. The spacecraft not only reached the surface but survived the touchdown and continued to send back signals.

Pictures obtained as the spacecraft moved ever closer to its landing resemble in their increasing detail those returned from Ranger impacts on the Moon. Here is a sequence obtained as NEAR approached a large crater (again, named Shoemaker after the dean of astrogeologists and expert on asteroids). The caption gives the spatial resolution achieved for each image.

NEAR sequence of images made during its daring landing; resolution: a = 1.2 km; b = 1.- km; c = 200 meteers; d = 100 m; e = 50 m; f = 100 m; g = 10 m; h = 20 m; g and h display large boulders.

Here is a NEAR descent image taken when the spacecraft was just 250 m (820 ft) from the surface. Rocks less than a meter in dimension are scattered on the surface, as had been expected.

An image of EROS' surface, long dimension is 12 meters, showing rock debris of several to less than 1 meter long, taken during the final descent of NEAR-Shoemaker.

Astonishingly, the gamma ray spectrometer on the spacecraft was not damaged. When its solar panels were arrayed so as to pick up sunlight and hence provide power, the spectrometer was turned on and data were collected from two depths. Here is one of the plots:

Plots of the gamma ray spectrometer readings from the NEAR spacecraft after it had survived the hard descent onto the surface of Eros; the insert is an artist's conception of the craft at the touch down site.

This triumph, with its serendipitous landing results, augers well for future missions to asteroid surfaces; sampling these (either by instrumental analysis or by sampling collecting and return to Earth) will give scientists their first solid data on the composition of these asteroids which have the most primitive material in the condensed planetary rock system. This should thus confirm whether any of the meteorites fallen on Earth were truly samples of the planetesimals which, for Earth and the inner planets, were the primary constituents that eventually melted.

As implied on page 18-3, the dinosaur "final solution" from a huge asteroidal impact, followed by several movies that deal with world-threatening (and destroying) collisions with outer space debris, have led to a more organized search and inventory (and orbit-determination) for asteroids and comets. Optical telescope methods look for tiny light blips in photographs that move with significant displacements relative to fixed star backgrounds. This is turning up new asteroidal bodies - many quite small - with notable numbers added each year. Another approach uses radar: this image of Toutalis (4.6 x 2.4 x1.9 km [2.9 x 1.5 x 1.2 miles]) is a mosaic of several radar returns:

The small asteroid Toutalis, imaged by an Earth-based radar.

19-73: What have you seen (as images) before in Section 19 that remind you of these asteroids? ANSWER

The question of the origin of asteroids is still debated. All agree that they represent primitive materials and are about as old as the planets. A few planetologists still argue that at least some, perhaps all, of those in the Main Belt represent a disrupted planet. But most subscribe to the concept that these are really planetesimals (accretionary bodies built up of fragments of gravity-attracted small solids that condensed and organized during the first stages of solar history) that never succeeded in building up by accretion into (a) planet(s). The reason for this failure to reach planet-size is ascribed to the perturbing influence of gravity from the Giant Jupiter. Most of these bodies today have undergone repeated collisions that knock off chunks from the target body, some of which escape to become new asteroids but much (most?) re-assemble into the collided remnant or into a neighboring asteroid to form a new shape.

Some asteroids are solid in the conventional sense but may now consist of joined fragments (note shape of Toutatis, which appears to have three connected pieces); these have greater densities but may contain internal voids. Others, perhaps the majority, being lower in density, are thought to be comprised of smaller fragments. These indeed may even be a composite of sand, gravel, and small boulder sized material (probably the residue of the carbonaceous silicates that were the first solar dust aggregates). They are held together by gravity, electrostatic attraction, and possibly a form of ice. When collisions on them occur, pieces may be knocked off but these tend to rejoin the parent in a matter of days. Over billions of years many collsions have occurred, reordering the asteroids into new assemblages. Most asteroidal surfaces, whether solid or held together in a manner similar to "sand castles" made at a beach, are covered with loose debris or "regolith".

In the treatment of meteorites (page 19-2) it was pointed out that asteroids ranged from primitive carbonaceous chondrites in composition to those that seem to have a distinct set of concentric shells, with iron cores. The stony meteorites display varying degrees of thermal and shock metamorphism, with the irons being evidence that the asteroidal body may have grown large enough to melt and form an iron core before later disruption. Sources of heat energy are needed to produce these differences. Some of that energy was provided by the same radioisotopes of uranium, thorium, and potassium as currently continue to heat the Earth. But in the early Solar System there were also isotopes with short half-lifes that may have produced even more thermal energy. Two known to have been effective are Al26 and Fe60, both now naturally extinct. Collisions between asteroidal bodies also contributed to the heat content, causing at least part of the target body to overheat locally. Another source of heat could have been from the Sun itself, both as thermal radiation and solar wind.

Asteroids, and fragments therefrom, occasionally hit the Earth, as we showed on page 19-2 dealing with meteorites and page 18-1 dealing with impact craters. So do comets strike our planet: a possible example (although it could have been a stony meteorite) was the 1908 Tunguska event in Siberia, where trees were knocked down (in a radial pattern pointing to a center of blast) over many hundreds of square kilometers by an explosion just above the surface. Great amounts of dust were thrown into the atmosphere, producing abnormal red sunsets worldwide for the next several years.

Comets are among the most spectacular of the heavenly bodies with their long, icy tail, receiving mystical significance from early observers, until later observers determined their true nature.

19-74: Name the comets that YOU have actually seen (through binoculars or telescope, or even naked eye) in your lifetime. ANSWER

We now know that comets are mainly ice balls of varying sizes (up to 10-30 km [6-19 miles]), mixed with rock debris to some extent. They travel in eccentric orbits (e.g., Kuiper belt) within the solar system, repeating appearances or simply flying through once, if not captured gravitationally. As seen when still far from Earth, the central coma appears as a glowing ball from 10,000 to 100,000 km (6,214-62,137 miles) in apparent diameter, around a much smaller solid nucleus. A good example is the comet Encke:

Comet Encke, as a coma, without any significant tail, seen through an Earth telescope.

As a comet passes the Sun, the solar wind and other factors cause it to ablate, expanding the coma and creating a stream of particles that trail off as a long tail (up to 100 million km [62,137,000 mi] long) of dust and plasma. The tail points away from the Sun along a radial line. Most comets actually develop two tails, one consisting of debris reflecting sunglight and the other composed of ions excited by UV irradiation. Look first at the unnamed comet and then at the tail from famed comet Halley.

Ion and dust tails emanating from the bright coma of a comet.

Halley’s Comet, with a well-developed tail, seen through a ground telescope in 1986.

Scientists think that the nucleus (descriptively referred to as a "dirty snowball") consists of very primitive materials, organized during the solar system's development. Spectroscopic studies indicate the presence of molecular compounds of carbon, nitrogen, and hydrogen, including CN, NH, NH2, and HCN, which break into ions carried into the tail. A telescope view of Comet Kudo-Fujikawa using a sensor that detects hydrogen ions produced this image, in which the H ions are colored reddish:

Comet Kudo-Fujikawa, with reddish tail enriched in hydrogen ions.

Astronomers know the orbits of some comets well enough (through observations) to predict when they will return. Most comets come from either the Kuiper Belt ( beyond Pluto) or the vast Oort "Clouds" that extend to the outer reaches of the solar system. Some may be intergalatic but that has yet to be demonstrated.

The Kuiper Belt contains Objects (KBO) that are primarily comets but seem to also include some asteroidal type bodies. The Belt was predicted to exist by Gerald Kuiper in the 1950s but the first direct imaging was not achieved until the 1990s. The example shown here indicates the difficulty in spotting such small objects far out in the Solar System; once located, the circled object moves relative to the background, allowing its orbital migration to be calculated.

A KBO, circled in black.

The KBOs are clustered in a disk-shaped region near the ecliptic (plane in which most of the planets orbit the Sun), lie at distances from 30 to 100 A.U., and may contain up to (an estimated) 100,000 objects larger than 20 km in diameter. Centaur-class KBOs are relatively close to Neptune's orbit and include the icy body named Chiron (discovered in 1977; at first thought to be an asteroid but now proved to be a comet with a short tail); of the estimated 400 Centaur objects greater than 100 km in diameter, at least 9 are notably larger.

The biggest known KBO asteroid is 2002 LM60, discovered first by a ground telescope (making it the farthest solar system object yet found) and then confirmed and studied by the Hubble Space Telescope. The discoverers have named this Quaoar (pronounced Kwa o whar), an American Indian name associated with the tribe that once occupied the Los Angeles Basin. The asteroid is spherical (indicating that it was once molten) and is close to 1250 km (780 miles in diameter). Quaoar is 6.5 billion kilometers from the Sun, around which it moves in a circular orbit. It lies 1.5 billion kilometers (about one billion miles) past Pluto. Another recently discovered asteroid is 2001 KX76, named Ixion, whose size ~1200 km (745 miles). The largest objects in this belt (using Pluto and its moon Charon for comparison) are depicted in this schematic:

Sizes of the largest asteroid-like objects in the Kuiper Belt, relative to Pluto.

Results of observations reported in 2003 by Rodney Gomez of Brazil support the presence of two distinct Kuiper belts. One lies largely within the solar ecliptic; its asteroids are grayish. A second belt has trajectories up to 40° off the ecliptic; its asteroids have a reddish tint.

The first attempt to land on an asteroid, collect samples, and return those to Esrth is being carried out by the Japanese space program. The small asteroid Itokawa has been reached by the Hayakawa

The Oort Cloud(OC) is a postulated swarm of perhaps billions of comets that orbit farther from the Sun than the KBOs. These orbits are not confined close to the ecliptic but can follow paths that occur anywhere in the "sphere" of the Solar System with the Sun at its center. As yet, no OC object has been imaged by either ground-based telescopes or the HST owing to their small sizes and great distances from Earth. However, their existence is based on firm reasoning that predicts them to be a significant part of the bodies that formed from the nebula that organized into the Sun, planets, and other objects. The artist's sketch below shows roughly the relative sizes of solar region volume containing the Oort Cloud and the Kuiper Belt:

The solar region in which the vastness of the Oort Cloud is compared to the Kuiper Belt.

As of 1995, 878 comets have been catalogued; most now have their orbits reasonably well calculated. Of these 184 have definitely been established as periodic (at intervals of years to centuries pass the inner Solar System as they orbit the Sun; these can be divided into Short-Period (KBO) and Long Period (OC) types; new comets and others of the 878 may also be periodic but more observations over time are needed to confirm this. The number of comets - most still undetected - within the Solar System may be in the trillions.

Most comets positioned well away from the Sun are without pronounced tails, and are best found by looking for notable displacements of small bright objects (early stage comas) relative to fixed star backgrounds in film records taken days apart. Such motions delineate the advance of comets, as well as reflecting asteroids, at high speeds through solar space.

The best known of all comets is Halley’s Comet, observed and recorded in ancient times. Its periodicity, first predicted by Edmund Halley to verify Newton's Laws of Motion, causes it to reappear about every 76 (range 75 to 79) years. Having passed in 1909, as shown in this wide angle view that displays its magnificent tail, it reappeared in 1986, and many predicted it would provide a great celestial display (which generally fell short of expectations).

Wide-angle camera photo of Halley taken during its close approach to Earth in 1909, as seen through a telescope.

Debate raged in advance about sending one or more space probes to examine it close-up, since the next opportunity would not be until 2061. Although NASA decided against this adventure, Japan, the former Soviet Union, and the European Space Agency sent probes to gather data. In particular, the Italian government designed and launched a spacecraft named Giotto, which came within 540 km (336 mi) of the nucleus on March 13, 1986. Here is a close approach view:

Close view of Halley’s nucleus as it was being approached by the Giotto spacecraft whose mission was to study this comet in 1986.

Giotta found that Halley's nucleus, measured at 16 km x 8 km (10 x 5 mi), is very dark, lumpy and of low density (0.1-0.2 g/cc). This suggests that it was then very porous, with most of the ice having ablated or evaporated away, leaving carbon-rich dust as a residue. Although not as bright as anticipated and a disappointment to ground viewers, the comet, as seen through telescopes, provided exceptional displays. We can emphasize reflectivity variations in its coma and tail, representing particle density differences, by displaying them in false color:

False color image showing the variations in coma and tail reflectivity of Halley's Comet.

A recent comet sensation is Comet Hale-Boggs, discovered on July 23, 1995, that passed Earth as close as 85 million miles on April 2, 1997. Hailed by many as the Comet of the Century because of its size (four times larger than Halley’s Comet) and brightness, it was visible in northern and southern hemispheres during much of the first half of 1997. Here is a typical view, taken on March 11, 1997, by Jerry Platt, one of many amateur astronomers who tracked this spectacular celestial visitor.

Color photograph of the comet Hale-Boggs, taken by an amateur astronomer, Jerry Platt, on March 11 1997.

Most of those that are far from the Sun don’t have pronounced tails, so to find them we look for notable displacements of small bright objects (early stage comas) relative to fixed star backgrounds in film records, taken days apart. Such motions delineate the advance of comets, as well as reflecting asteroids, at high speeds through the solar system. The 6 panels in the next illustration show the progressive movement over hours of the comet Wirtanen (when imaged it was about 605 million km - or more than 4 A.U's - from Earth. The comet, a tiny dot is circled in each panel. Follow its displacement from right to left (in panel 4 it is directly in front of the reference background star).

A time sequence of telescope photos showing the leftward movement of the Comet Wirtaten past a reference star.

In 1999, NASA sent a probe called Deep Space 1 to test new observation techniques and if possible to gather new information about comets it would approach. It has lasted beyond its planned lifetime. One of its most spectacular achievements was on Sept. 22, 2001 when it passed within 2200 km (1400 miles) of the Comet Borrelly to image its nucleus. Concern was high that the probe, suffering now from some malfunctions, would be damaged by cometary debris. However, it succeeded grandly in getting excellent images of the nucleus. Below is the last image received before planned shutdown in which the elongated nucleus, an 8 km (5 mile) long object imaged at 45 m resolution, displays ridgelike irregularities, faults and other geologically describable features; in some ways, it resembles an asteroid but its dark surface is composed of ice and dust (note the jets of material streaming off):

The nucleus of Comet Borrelly, imaged by the Deep Space 1 probe.

Sensors on Deep Space 1 produced these images, with information described in their captions.

Color-coded image of Comet Borrelly and its surrounding excited ions including those in a short tail.

The hot plasma of solar wind-excited ions around Borrelly.

Solar wind-induced excitation of material coming off of Comet Borrelly; the big dip in the spectrum is due to water released from the comet

A relatively pristine comet was discovered in January 1988 by the Swiss astronomer Paul Wild (given its German pronunciation as "Vilt"). Comet Wild 2 was once beyond Jupiter but a close encounter with Jupiter has carried it into an orbit beyond Mars such that it passes Earth about every 6 years. Here is its appearance in December 1990:

Comet Wild 2.

In 2001, NASA launched a probe (the Stardust mission) to image Comet Wild 2 and to collect samples of dust and gas as it passed through the comet's tail. This drawing shows how the particles will be collected:

The Stardust probe.

The spacecraft will return these dust samples to Earth in January of 2006. Here is a view of Wild 2's nucleus (~5.4 km [3.3 miles] in maximum dimension) from a distance of 500 km (341 miles):

The nucleus of Comet Wild 2.

Features on Wild 2 have been named (with descriptive humor), as shown here, in which the spacecraft was somewhat closer.

Named features on Wild 2.

Close-up images show some distinctive features, including depressions, fractures, and prominences

Features on Wild 2.

Still another image subjected to different processing showed glowing material coming off this nucleus. The cometary body apppears to consist of a mix of ice and rock together hard enought to serve as a strong solid that is not disrupted by repeated cratering action (some investigators think the pits are ablation- rather than impact-produced).

Glowing jets of material coming off Comet Wild.

Using photometric filters, Stardust has obtained data in the visible and infrared allowing good estimates of the composition of materials at Wild 2's surface, as follows:

Compositional components at Wild 2's surface.

The interpretation of Wild 2's makeup indicates that it has some similiarities to the Kuiper belt asteroids, suggesting some kinship.

The European Space Agency (ESA) is conducting a follow-up to Giotto with a mission (Rosetta) to the Comet Churyumov-Gerusmanko (6 km diameter) after a successful launch on March 2, 2004 and planned arrival in 2014. Heavily instrumented, Rosetta includes a lander on the comet's nucleus.

19-75: How do you think comets have influenced the Earth in history? ANSWER

What is the ultimate fate of most comets? Two possibilties are most likely. First, they may just gradually "wear away" as their icy comas are ablated or otherwise destroyed as they repeatedly pass their parent star. Second, they may be pulled into that star or one of its planets (see next page) by gravitational attraction, thus becoming totally annihilated. Evidence for this latter fate has been indirectly retrieved from a ground telescope study (McDonald Observatory in Texas) of a Herbig Be type star, LKHa234 in nebular cloud NGC 7129, 3200 l.y. away from Earth in the Milky Way (see page 20-5 for a discussion of this star type). This 100000 year-old star (about 5 solar masses) was observed over 5 days. Spectra taken of it show dramatic changes, e.g., in sodium light, during that period. One reasonable interpretation is that a comet with sodium content crashed into the star, thus dispersing its source so that sodium spectral lines disappeared. Here is an image of LKHa234 and its surrounding nebula taken during this period.

LKHa234, a young Herbig Be star, some 3200 l.y. away; arrow points to star but the smaller round object near it is still too big to be a comet.

In the last twenty years or so, concern has heightened that asteroids or comets might strike the Earth, as was proved in Section 18. Those whose orbits could cross Earth are collectively known as Near-Earth Objects (or NEOs). This possibility was heightened by the comet that struck Jupiter, as discussed on the next page. Some federal and private funding has been provided to conduct a systematic search for NEOs. To date hundreds of new asteroids and a few comets have been detected and their orbits calculated. If one is shown to have a good chance to hit the Earth, several ways to stop this have been considered. Sending a space probe with a nuclear device onto the NEO might break it up, but the pieces could continue (like buckshot) on a collision course. The best strategy would be find a way to deflect the orbital path so that the asteroid or comet would have a much reduced chance of meeting the Earth in its orbit. A nuclear explosion away from the NEO could exert enough pressure to modify its orbit. Since calculations have now indicated that an Earth-striking NEO's impact strong enough to cause serious damage may be as frequent as once every thousand years, the NEO detection program has taken on a new urgency.

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Primary Author: Nicholas M. Short, Sr. email: nmshort@ptd.net