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Cosmic dust
Cosmic dust
Cosmic dust
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Porous chondrite dust particle

Cosmic dust – also called extraterrestrial dust, space dust, or star dust – is dust that occurs in outer space or has fallen onto Earth.[1][2] Most cosmic dust particles measure between a few molecules and 0.1 mm (100 μm), such as micrometeoroids (<30 μm) and meteoroids (>30 μm).[3] Cosmic dust can be further distinguished by its astronomical location: intergalactic dust, interstellar dust, interplanetary dust (as in the zodiacal cloud), and circumplanetary dust (as in a planetary ring). There are several methods to obtain space dust measurement.

In the Solar System, interplanetary dust causes the zodiacal light. Solar System dust includes comet dust, planetary dust (like from Mars),[4] asteroidal dust, dust from the Kuiper belt, and interstellar dust passing through the Solar System. Thousands of tons of cosmic dust are estimated to reach Earth's surface every year,[5] with most grains having a mass between 10−16 kg (0.1 pg) and 10−4 kg (0.1 g).[5] The density of the dust cloud through which the Earth is traveling is approximately 10−6 dust grains/m3.[6]

Cosmic dust contains some complex organic compounds (amorphous organic solids with a mixed aromatic–aliphatic structure) that could be created naturally, and rapidly, by stars.[7][8][9] A smaller fraction of dust in space is "stardust" consisting of larger refractory minerals that condensed as matter left by stars.

Interstellar dust particles were collected by the Stardust spacecraft and samples were returned to Earth in 2006.[10][11][12][13]

Study and importance

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Artist's impression of dust formation around a supernova explosion.[14]

Cosmic dust was once solely an annoyance to astronomers, as it obscures objects they wished to observe. When infrared astronomy began, the dust particles were observed to be significant and vital components of astrophysical processes. Their analysis can reveal information about phenomena like the formation of the Solar System.[15] For example, cosmic dust can drive the mass loss when a star is nearing the end of its life, play a part in the early stages of star formation, and form planets. In the Solar System, dust plays a major role in the zodiacal light, Saturn's B Ring spokes, the outer diffuse planetary rings at Jupiter, Saturn, Uranus and Neptune, and comets.

Zodiacal light caused by cosmic dust.[16]

The interdisciplinary study of dust brings together different scientific fields: physics (solid-state, electromagnetic theory, surface physics, statistical physics, thermal physics), fractal mathematics, surface chemistry on dust grains, meteoritics, as well as every branch of astronomy and astrophysics.[17] These disparate research areas can be linked by the following theme: the cosmic dust particles evolve cyclically; chemically, physically and dynamically. The evolution of dust traces out paths in which the Universe recycles material, in processes analogous to the daily recycling steps with which many people are familiar: production, storage, processing, collection, consumption, and discarding.

Observations and measurements of cosmic dust in different regions provide an important insight into the Universe's recycling processes; in the clouds of the diffuse interstellar medium, in molecular clouds, in the circumstellar dust of young stellar objects, and in planetary systems such as the Solar System, where astronomers consider dust as in its most recycled state. The astronomers accumulate observational 'snapshots' of dust at different stages of its life and, over time, form a more complete movie of the Universe's complicated recycling steps.

Parameters such as the particle's initial motion, material properties, intervening plasma and magnetic field determined the dust particle's arrival at the dust detector. Slightly changing any of these parameters can give significantly different dust dynamical behavior. Therefore, one can learn about where that object came from, and what is (in) the intervening medium.

Detection methods

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Cosmic dust of the Andromeda Galaxy as revealed in infrared light by the Spitzer Space Telescope.

A wide range of methods is available to study cosmic dust. Cosmic dust can be detected by remote sensing methods that utilize the radiative properties of cosmic dust particles, cf. Zodiacal light measurement.

Cosmic dust can also be detected directly ('in-situ') using a variety of collection methods and from a variety of collection locations. Estimates of the daily influx of extraterrestrial material entering the Earth's atmosphere range between 5 and 300 tonnes.[18][19]

NASA collects samples of star dust particles in the Earth's atmosphere using plate collectors under the wings of stratospheric-flying airplanes. Dust samples are also collected from surface deposits on the large Earth ice-masses (Antarctica and Greenland/the Arctic) and in deep-sea sediments.

Don Brownlee at the University of Washington in Seattle first reliably identified the extraterrestrial nature of collected dust particles in the latter 1970s. Another source is the meteorites, which contain stardust extracted from them. Stardust grains are solid refractory pieces of individual presolar stars. They are recognized by their extreme isotopic compositions, which can only be isotopic compositions within evolved stars, prior to any mixing with the interstellar medium. These grains condensed from the stellar matter as it cooled while leaving the star.

Cosmic dust of the Horsehead Nebula as revealed by the Hubble Space Telescope.

In interplanetary space, dust detectors on planetary spacecraft have been built and flown, some are presently flying, and more are presently being built to fly. The large orbital velocities of dust particles in interplanetary space (typically 10–40 km/s) make intact particle capture problematic. Instead, in-situ dust detectors are generally devised to measure parameters associated with the high-velocity impact of dust particles on the instrument, and then derive physical properties of the particles (usually mass and velocity) through laboratory calibration (i.e., impacting accelerated particles with known properties onto a laboratory replica of the dust detector). Over the years dust detectors have measured, among others, the impact light flash, acoustic signal and impact ionisation. Recently the dust instrument on Stardust captured particles intact in low-density aerogel.

Dust detectors in the past flew on the HEOS 2, Helios, Pioneer 10, Pioneer 11, Giotto, Galileo, Ulysses and Cassini space missions, on the Earth-orbiting LDEF, EURECA, and Gorid satellites, and some scientists have utilized the Voyager 1 and 2 spacecraft as giant Langmuir probes to directly sample the cosmic dust. Presently dust detectors are flying on the Ulysses, Proba, Rosetta, Stardust, and the New Horizons spacecraft. The collected dust at Earth or collected further in space and returned by sample-return space missions is then analyzed by dust scientists in their respective laboratories all over the world. One large storage facility for cosmic dust exists at the NASA Houston JSC.

Infrared light can penetrate cosmic dust clouds, allowing us to peer into regions of star formation and the centers of galaxies. NASA's Spitzer Space Telescope was the largest infrared space telescope, before the launch of the James Webb Space Telescope. During its mission, Spitzer obtained images and spectra by detecting the thermal radiation emitted by objects in space between wavelengths of 3 and 180 micrometres. Most of this infrared radiation is blocked by the Earth's atmosphere and cannot be observed from the ground. Findings from the Spitzer have revitalized the studies of cosmic dust. One report showed some evidence that cosmic dust is formed near a supermassive black hole.[20]

Astronomers used the James Webb Space Telescope to image the warm dust around a nearby young star, Fomalhaut, in order to study the first asteroid belt ever seen outside of the Solar System in infrared light.[21]

Another detection mechanism is polarimetry. Dust grains are not spherical and tend to align to interstellar magnetic fields, preferentially polarizing starlight that passes through dust clouds. In nearby interstellar space, where interstellar reddening is not intense enough to be detected, high precision optical polarimetry has been used to glean the structure of dust within the Local Bubble.[22]

In 2019, researchers found interstellar dust in Antarctica which they relate to the Local Interstellar Cloud. The detection of interstellar dust in Antarctica was done by the measurement of the radionuclides iron-60 and manganese-53 by highly sensitive Accelerator mass spectrometry.[23]

Radiation properties

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HH 151 is a bright jet of glowing material trailed by an intricate, orange-hued plume of gas and dust.[24]

A dust particle interacts with electromagnetic radiation in a way that depends on its cross section, the wavelength of the electromagnetic radiation, and on the nature of the grain: its refractive index, size, etc. The radiation process for an individual grain is called its emissivity, dependent on the grain's efficiency factor. Further specifications regarding the emissivity process include extinction, scattering, absorption, or polarisation. In the radiation emission curves, several important signatures identify the composition of the emitting or absorbing dust particles.

Dust particles can scatter light nonuniformly. Forward scattered light is light that is redirected slightly off its path by diffraction, and back-scattered light is reflected light.

The scattering and extinction ("dimming") of the radiation gives useful information about the dust grain sizes. For example, if the object(s) in one's data is many times brighter in forward-scattered visible light than in back-scattered visible light, then it is understood that a significant fraction of the particles are about a micrometer in diameter.

The scattering of light from dust grains in long exposure visible photographs is quite noticeable in reflection nebulae, and gives clues about the individual particle's light-scattering properties. In X-ray wavelengths, many scientists are investigating the scattering of X-rays by interstellar dust, and some have suggested that astronomical X-ray sources would possess diffuse haloes, due to the dust.[25]

Presolar grains

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Main article: Presolar grains

Presolar grains are contained within meteorites, from which they are extracted in terrestrial laboratories. The term "stardust" or "presolar stardust" is sometimes used to distinguish grains from a single star in comparison to aggregated interstellar dust particles, though this distinction is not universally applied.[26][27] Presolar material was a component of the dust in the interstellar medium before its incorporation into meteorites. The meteorites have stored those presolar grains ever since the meteorites first assembled within the planetary accretion disk more than four billion years ago. Carbonaceous chondrites are especially fertile reservoirs of presolar material. Presolar grains definitionally existed before the Earth was formed. Presolar grain (and, less frequently, "stardust" or "presolar stardust") is the scientific term referring to refractory dust grains that condensed from cooling ejected gases from individual presolar stars and incorporated into the cloud from which the Solar System condensed.[28]

Many different types of presolar grains have been identified by laboratory measurements of the highly unusual isotopic composition of the chemical elements that comprise each presolar grain. These refractory mineral grains may earlier have been coated with volatile compounds, but those are lost in the dissolving of meteorite matter in acids, leaving only insoluble refractory minerals. Finding the grain cores without dissolving most of the meteorite has been possible, but difficult and labor-intensive.

Many new aspects of nucleosynthesis have been discovered from the isotopic ratios within the presolar grains.[29] An important property of presolar is the hard, refractory, high-temperature nature of the grains. Prominent are silicon carbide, graphite, aluminium oxide, aluminium spinel, and other such solids that would condense at high temperature from a cooling gas, such as in stellar winds or in the decompression of the inside of a supernova. They differ greatly from the solids formed at low temperature within the interstellar medium.

Also important are their extreme isotopic compositions, which are expected to exist nowhere in the interstellar medium. This also suggests that the presolar grains condensed from the gases of individual stars before the isotopes could be diluted by mixing with the interstellar medium. These allow the source stars to be identified. For example, the heavy elements within the silicon carbide (SiC) grains are almost pure S-process isotopes, fitting their condensation within AGB star red giant winds inasmuch as the AGB stars are the main source of S-process nucleosynthesis and have atmospheres observed by astronomers to be highly enriched in dredged-up s process elements.

Another dramatic example is given by supernova condensates, usually shortened by acronym to SUNOCON (from SUperNOva CONdensate[28]) to distinguish them from other grains condensed within stellar atmospheres. SUNOCONs contain in their calcium an excessively large abundance[30] of 44Ca, demonstrating that they condensed containing abundant radioactive 44Ti, which has a 65-year half-life. The outflowing 44Ti nuclei were thus still "alive" (radioactive) when the SUNOCON condensed near one year within the expanding supernova interior, but would have become an extinct radionuclide (specifically 44Ca) after the time required for mixing with the interstellar gas. Its discovery proved the prediction[31] from 1975 that it might be possible to identify SUNOCONs in this way. The SiC SUNOCONs (from supernovae) are only about 1% as numerous as are SiC stardust from AGB stars.

Stardust itself (SUNOCONs and AGB grains that come from specific stars) is but a modest fraction of the condensed cosmic dust, forming less than 0.1% of the mass of total interstellar solids. The high interest in presolar grains derives from new information that it has brought to the sciences of stellar evolution and nucleosynthesis.

Laboratories have studied solids that existed before the Earth was formed.[32] This was once thought impossible, especially in the 1970s when cosmochemists were confident that the Solar System began as a hot gas[33] virtually devoid of any remaining solids, which would have been vaporized by high temperature. The existence of presolar grains proved this historic picture incorrect.

Some bulk properties

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Smooth chondrite interplanetary dust particle.

Cosmic dust is made of dust grains and aggregates into dust particles. These particles are irregularly shaped, with porosity ranging from fluffy to compact. The composition, size, and other properties depend on where the dust is found, and conversely, a compositional analysis of a dust particle can reveal much about the dust particle's origin. General diffuse interstellar medium dust, dust grains in dense clouds, planetary rings dust, and circumstellar dust, are each different in their characteristics. For example, grains in dense clouds have acquired a mantle of ice and on average are larger than dust particles in the diffuse interstellar medium. Interplanetary dust particles (IDPs) are generally larger still.

Major elements of 200 stratospheric interplanetary dust particles.

Most of the influx of extraterrestrial matter that falls onto the Earth is dominated by meteoroids with diameters in the range 50 to 500 micrometers, of average density 2.0 g/cm3 (with porosity about 40%). The total influx rate of meteoritic sites of most IDPs captured in the Earth's stratosphere range between 1 and 3 g/cm3, with an average density at about 2.0 g/cm3.[34]

Other specific dust properties: in circumstellar dust, astronomers have found molecular signatures of CO, silicon carbide, amorphous silicate, polycyclic aromatic hydrocarbons, water ice, and polyformaldehyde, among others (in the diffuse interstellar medium, there is evidence for silicate and carbon grains). Cometary dust is generally different (with overlap) from asteroidal dust. Asteroidal dust resembles carbonaceous chondritic meteorites. Cometary dust resembles interstellar grains which can include silicates, polycyclic aromatic hydrocarbons, and water ice.

In September 2020, evidence was presented of solid-state water in the interstellar medium, and particularly, of water ice mixed with silicate grains in cosmic dust grains.[35]

Cosmic dust grains can exhibit porous structures, which influence chemical processes in astrophysical environments and highlight the importance of including porosity in dust models.[36]

Dust grain formation

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For the first time, the NASA / ESA / Canadian Space Agency / James Webb Space Telescope has observed the chemical signature of carbon-rich dust grains at redshift z ≈ 7, which is roughly equivalent to one billion years after the birth of the Universe, this observation suggests exciting avenues of investigation into both the production of cosmic dust and the earliest stellar populations in our Universe.

The large grains in interstellar space are probably complex, with refractory cores that condensed within stellar outflows topped by layers acquired during incursions into cold dense interstellar clouds. That cyclic process of growth and destruction outside of the clouds has been modeled[37][38] to demonstrate that the cores live much longer than the average lifetime of dust mass. Those cores mostly start with silicate particles condensing in the atmospheres of cool, oxygen-rich red-giants and carbon grains condensing in the atmospheres of cool carbon stars. Red giants have evolved or altered off the main sequence and have entered the giant phase of their evolution and are the major source of refractory dust grain cores in galaxies. Those refractory cores are also called stardust (section above), which is a scientific term for the small fraction of cosmic dust that condensed thermally within stellar gases as they were ejected from the stars. Several percent of refractory grain cores have condensed within expanding interiors of supernovae, a type of cosmic decompression chamber. Meteoriticists who study refractory stardust (extracted from meteorites) often call it presolar grains but that within meteorites is only a small fraction of all presolar dust. Stardust condenses within the stars via considerably different condensation chemistry than that of the bulk of cosmic dust, which accretes cold onto preexisting dust in dark molecular clouds of the galaxy. Those molecular clouds are very cold, typically less than 50K, so that ices of many kinds may accrete onto grains, in cases only to be destroyed or split apart by radiation and sublimation into a gas component. Finally, as the Solar System formed many interstellar dust grains were further modified by coalescence and chemical reactions in the planetary accretion disk. The history of the various types of grains in the early Solar System is complicated and only partially understood.

Astronomers know that the dust is formed in the envelopes of late-evolved stars from specific observational signatures. In infrared light, emission at 9.7 micrometres is a signature of silicate dust in cool evolved oxygen-rich giant stars. Emission at 11.5 micrometres indicates the presence of silicon carbide dust in cool evolved carbon-rich giant stars. These help provide evidence that the small silicate particles in space came from the ejected outer envelopes of these stars.[39][40]

Conditions in interstellar space are generally not suitable for the formation of silicate cores. This would take excessive time to accomplish, even if it might be possible. The arguments are that: given an observed typical grain diameter a, the time for a grain to attain a, and given the temperature of interstellar gas, it would take considerably longer than the age of the Universe for interstellar grains to form.[41] On the other hand, grains are seen to have recently formed in the vicinity of nearby stars, in nova and supernova ejecta, and in R Coronae Borealis variable stars which seem to eject discrete clouds containing both gas and dust. So mass loss from stars is unquestionably where the refractory cores of grains formed.

Most dust in the Solar System is highly processed dust, recycled from the material out of which the Solar System formed and subsequently collected in the planetesimals, and leftover solid material such as comets and asteroids, and reformed in each of those bodies' collisional lifetimes. During the Solar System's formation history, the most abundant element was (and still is) H2. The metallic elements: magnesium, silicon, and iron, which are the principal ingredients of rocky planets, condensed into solids at the highest temperatures of the planetary disk. Some molecules such as CO, N2, NH3, and free oxygen, existed in a gas phase. Some molecules, for example, graphite (C) and SiC would condense into solid grains in the planetary disk; but carbon and SiC grains found in meteorites are presolar based on their isotopic compositions, rather than from the planetary disk formation. Some molecules also formed complex organic compounds and some molecules formed frozen ice mantles, of which either could coat the "refractory" (Mg, Si, Fe) grain cores. Stardust once more provides an exception to the general trend, as it appears to be totally unprocessed since its thermal condensation within stars as refractory crystalline minerals. The condensation of graphite occurs within supernova interiors as they expand and cool, and do so even in gas containing more oxygen than carbon,[42] a surprising carbon chemistry made possible by the intense radioactive environment of supernovae. This special example of dust formation has merited specific review.[43]

Planetary disk formation of precursor molecules was determined, in large part, by the temperature of the solar nebula. Since the temperature of the solar nebula decreased with heliocentric distance, scientists can infer a dust grain's origin(s) with knowledge of the grain's materials. Some materials could only have been formed at high temperatures, while other grain materials could only have been formed at much lower temperatures. The materials in a single interplanetary dust particle often show that the grain elements formed in different locations and at different times in the solar nebula. Most of the matter present in the original solar nebula has since disappeared; drawn into the Sun, expelled into interstellar space, or reprocessed, for example, as part of the planets, asteroids or comets.

Due to their highly processed nature, IDPs (interplanetary dust particles) are fine-grained mixtures of thousands to millions of mineral grains and amorphous components. We can picture an IDP as a "matrix" of material with embedded elements which were formed at different times and places in the solar nebula and before the solar nebula's formation. Examples of embedded elements in cosmic dust are GEMS, chondrules, and CAIs.

From the solar nebula to Earth

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A dusty trail from the early Solar System to carbonaceous dust today.

The arrows in the adjacent diagram show one possible path from a collected interplanetary dust particle back to the early stages of the solar nebula.

We can follow the trail to the right in the diagram to the IDPs that contain the most volatile and primitive elements. The trail takes us first from interplanetary dust particles to chondritic interplanetary dust particles. Planetary scientists classify chondritic IDPs in terms of their diminishing degree of oxidation so that they fall into three major groups: the carbonaceous, the ordinary, and the enstatite chondrites. As the name implies, the carbonaceous chondrites are rich in carbon, and many have anomalies in the isotopic abundances of H, C, N, and O.[44] From the carbonaceous chondrites, we follow the trail to the most primitive materials. They are almost completely oxidized and contain the lowest condensation temperature elements ("volatile" elements) and the largest amount of organic compounds. Therefore, dust particles with these elements are thought to have been formed in the early life of the Solar System. The volatile elements have never seen temperatures above about 500 K, therefore, the IDP grain "matrix" consists of some very primitive Solar System material. Such a scenario is true in the case of comet dust.[45] The provenance of the small fraction that is stardust (see above) is quite different; these refractory interstellar minerals thermally condense within stars, become a small component of interstellar matter, and therefore remain in the presolar planetary disk. Nuclear damage tracks are caused by the ion flux from solar flares. Solar wind ions impacting on the particle's surface produce amorphous radiation damaged rims on the particle's surface. And spallogenic nuclei are produced by galactic and solar cosmic rays. A dust particle that originates in the Kuiper Belt at 40 AU would have many more times the density of tracks, thicker amorphous rims and higher integrated doses than a dust particle originating in the main-asteroid belt.

Based on 2012 computer model studies, the complex organic molecules necessary for life (extraterrestrial organic molecules) may have formed in the protoplanetary disk of dust grains surrounding the Sun before the formation of the Earth.[46] According to the computer studies, this same process may also occur around other stars that acquire planets.[46]

In September 2012, NASA scientists reported that polycyclic aromatic hydrocarbons (PAHs), subjected to interstellar medium (ISM) conditions, are transformed, through hydrogenation, oxygenation and hydroxylation, to more complex organics – "a step along the path toward amino acids and nucleotides, the raw materials of proteins and DNA, respectively".[47][48] Further, as a result of these transformations, the PAHs lose their spectroscopic signature which could be one of the reasons "for the lack of PAH detection in interstellar ice grains, particularly the outer regions of cold, dense clouds or the upper molecular layers of protoplanetary disks."[47][48]

In February 2014, NASA announced a greatly upgraded database[49][50] for detecting and monitoring polycyclic aromatic hydrocarbons (PAHs) in the universe. According to NASA scientists, over 20% of the carbon in the Universe may be associated with PAHs, possible starting materials for the formation of life.[50] PAHs seem to have been formed shortly after the Big Bang, are abundant in the Universe,[51][52][53] and are associated with new stars and exoplanets.[50]

In March 2015, NASA scientists reported that, for the first time, complex DNA and RNA organic compounds of life, including uracil, cytosine and thymine, have been formed in the laboratory under outer space conditions, using starting chemicals, such as pyrimidine, found in meteorites. Pyrimidine, like polycyclic aromatic hydrocarbons (PAHs), the most carbon-rich chemical found in the Universe, may have been formed in red giants or in interstellar dust and gas clouds, according to the scientists.[54]

Some "dusty" clouds in the universe

[edit]
The Shark Nebula is a dark cloud reflection nebula in the constellation Cepheus.

The Solar System has its own interplanetary dust cloud, as do extrasolar systems. There are different types of nebulae with different physical causes and processes: diffuse nebula, infrared (IR) reflection nebula, supernova remnant, molecular cloud, HII regions, photodissociation regions, and dark nebula.

Distinctions between those types of nebula are that different radiation processes are at work. For example, H II regions, like the Orion Nebula, where a lot of star-formation is taking place, are characterized as thermal emission nebulae. Supernova remnants, on the other hand, like the Crab Nebula, are characterized as nonthermal emission (synchrotron radiation).

Some of the better known dusty regions in the Universe are the diffuse nebulae in the Messier catalog, for example: M1, M8, M16, M17, M20, M42, M43.[55]

Some larger dust catalogs are Sharpless (1959) A Catalogue of HII Regions, Lynds (1965) Catalogue of Bright Nebulae, Lynds (1962) Catalogue of Dark Nebulae, van den Bergh (1966) Catalogue of Reflection Nebulae, Green (1988) Rev. Reference Cat. of Galactic SNRs, The National Space Sciences Data Center (NSSDC),[56] and CDS Online Catalogs.[57]

Dust sample return

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The Discovery program's Stardust mission, was launched on 7 February 1999 to collect samples from the coma of comet Wild 2, as well as samples of cosmic dust. It returned samples to Earth on 15 January 2006. In 2007, the recovery of particles of interstellar dust from the samples was announced.[58]

Dust particles on Earth

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In 2017, Genge et al published a paper about "urban collection" of dust particles on Earth. The team were able to collect 500 micrometeorites from rooftops. Dust was collected in Oslo and in Paris, and "all particles are silicate-dominated (S type) cosmic spherules with subspherical shapes that form by melting during atmospheric entry and consist of quench crystals of magnesian olivine, relict crystals of forsterite, and iron-bearing olivine within glass".[59] In the UK, scientists look for micrometeorites on the rooftops of cathedrals, like Canterbury Cathedral and Rochester Cathedral.[60] Currently 40,000 tons of cosmic dust fall to Earth each year.[61]

See also

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References

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Further reading

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Revisions and contributorsEdit on WikipediaRead on Wikipedia

Cosmic dust

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Cosmic dust consists of tiny solid particles, typically ranging from a few nanometers to several micrometers in diameter, dispersed throughout the in regions such as the , interplanetary space, and around . These grains are primarily composed of refractory materials like silicates and carbonaceous compounds (such as and polycyclic aromatic hydrocarbons), often coated with volatile ices including , , and . Formed mainly in the outflows of evolved like (AGB) and supernovae, cosmic dust plays a crucial role in the cosmic cycle by recycling elements and facilitating the formation of molecules, , and . In the interstellar medium, dust grains constitute about 1% of the total mass, with a gas-to-dust mass ratio of approximately 100:1, making them a minor but influential component. They absorb and scatter ultraviolet and visible light from stars, causing that reddens starlight and obscures distant objects, while re-emitting the absorbed energy as thermal radiation. This property has historically challenged astronomers but is now leveraged by telescopes like NASA's to peer through dusty regions. Recent observations have detected carbon-rich dust in galaxies as early as 800 million years after the and suggest dust grains may be fluffier than previously thought, enhancing insights into early cosmic chemistry. Dust also polarizes light due to its non-spherical shapes and alignment with magnetic fields, providing insights into interstellar magnetic fields and grain properties. The origins and evolution of cosmic dust are tied to and galactic chemical enrichment. Heavy elements forged in condense into dust grains when cooling gases in stellar atmospheres or remnants reach temperatures below about 1,227°C (2,240°F). Over time, grains grow through accretion and coagulation in dense clouds, but they are also destroyed by shocks from supernovae or , maintaining a dynamic balance. In protoplanetary disks, dust aggregation leads to formation, directly contributing to the building blocks of planets like , where cosmic dust influx delivers essential volatiles and organics. Approximately 5,000 to 7,000 tons (about 14-19 tons per day, as of 2021 estimates) of such dust enters Earth's atmosphere annually, influencing and potentially contributing to life's origins. Beyond astronomy, cosmic dust serves as a probe of galactic history, with isotopic compositions revealing past stellar events and dust production in the early universe beginning as early as about 700 million years after the Big Bang, as detected in distant galaxies. Missions like NASA's Stardust and Cassini have collected and analyzed extraterrestrial dust, confirming diverse compositions from comets, asteroids, and interstellar sources. Understanding dust's role is vital for modeling star formation rates, galaxy evolution, and even the distribution of habitable zones in the cosmos.

Definition and Properties

Composition and Structure

Cosmic dust grains are composed primarily of silicates, such as ((Mg,Fe)₂SiO₄) and (MgSiO₃), which form the core of many particles and account for a significant fraction of the interstellar mass. Carbonaceous materials, including and polycyclic aromatic hydrocarbons (PAHs), constitute another major component, with PAHs featuring aromatic structures of tens to hundreds of carbon atoms that contribute to emission features. In colder regions like dense molecular clouds, volatile ices mantle these cores, dominated by (H₂O) with admixtures of CO, CO₂ (at ratios up to ~0.13 relative to H₂O), and other molecules such as CH₄ and NH₃. and sulfides, including iron (Fe) and iron sulfides, are also present, often incorporated into glassy structures or as inclusions within silicates. The internal architecture of cosmic dust grains varies widely, with silicates predominantly in amorphous forms (>95% of cases) though crystalline variants exist, particularly in certain circumstellar environments. Grains can be compact or highly porous, the latter featuring aggregates with void fractions up to 70-99% that enhance surface reactivity and light scattering properties. In dense interstellar clouds, a core-mantle prevails, where cores of silicates or carbon are coated by thick icy mantles that segregate molecules and influence grain evolution. Grain sizes span from sub-nanometer clusters (as small as ~1 nm for PAHs or nanodiamonds) to typical dimensions of 0.1-1 μm for individual particles, with rare fluffy aggregates reaching up to 100 μm through . Presolar grains, preserved in meteorites, exhibit distinctive isotopic signatures from , such as enhanced ¹⁷O/¹⁶O or depleted ¹⁸O/¹⁶O ratios in derived from oxygen-rich stars, and extreme ¹³C/¹²C enrichments in grains. These anomalies, often exceeding solar values by factors of 10-1000, provide direct evidence of heterogeneous grain formation in diverse stellar environments. A 2020 analysis of carbonaceous meteorites like Murchison and Tagish Lake has revealed hybrid organic-inorganic compositions, including (HMT) at concentrations up to 846 ppb integrated into matrices, highlighting the interplay of interstellar organics with components.

Physical Characteristics

Cosmic dust particles typically range in size from nanometers to micrometers, with the of grains following a power-law distribution, such as the Mathis-Rumpl-Nordsieck (MRN) model where n(a)∝a−3.5n(a) \propto a^{-3.5} for grain aa between approximately 0.005 and 0.25 μm; this distribution accounts for the observed of across to wavelengths. The of these particles varies from 0.5 to 3 g/cm³, influenced by their material composition, while high —reaching up to 90% in fluffy aggregate structures—lowers the effective and enhances properties like absorption and collisional interactions. In the , grains acquire a net negative charge ranging from -1 to -10 elementary charges due to the interplay of UV photoemission, which removes electrons and promotes positive charging, and more frequent collisions with plasma electrons that dominate the process. Temperatures of interstellar dust grains generally fall between 10 and 100 in with the ambient radiation field, though proximity to stars or embedded heating sources can elevate them to around 1000 . The residence time of cosmic dust in the is estimated at about 10810^8 years before destruction, mainly through and erosion in supernova shock waves.

Formation and Sources

Stellar and Supernova Origins

Cosmic dust grains primarily form through condensation processes in the outflows of asymptotic giant branch (AGB) stars, where cool, oxygen-rich or carbon-rich envelopes facilitate the nucleation of refractory materials. In oxygen-rich AGB stars, silicates such as forsterite (Mg₂SiO₄) and enstatite (MgSiO₃) condense at temperatures around 700–1000 K, while in carbon-rich AGB stars, amorphous carbon and silicon carbide (SiC) grains form at slightly higher temperatures of approximately 1400–1700 K. These processes occur in the extended stellar atmospheres, driven by thermal pulses that enhance mass loss and elemental mixing, leading to supersaturation and grain growth. Mass loss rates during this phase can reach up to 10⁻⁴ M⊙ yr⁻¹, enabling the ejection of significant dust quantities into the surrounding medium. Type II supernovae, arising from the core-collapse of massive stars (≳8 M⊙), represent another key source of cosmic dust, with grains forming rapidly in the cooling ejecta post-explosion. In these events, , aluminum (Al), and iron (Fe)-bearing grains, including silicates, , and , condense as the ejecta temperature drops from ~2000 K to below 1000 K within months. Models indicate that each Type II supernova can eject 0.1–1 M⊙ of dust, though observed masses are often lower (∼0.01–0.1 M⊙) due to destruction by reverse shocks in supernova remnants. and metal oxides dominate in many cases, reflecting the elemental abundances in the progenitor's envelope. Dust grains from both AGB stars and supernovae are dispersed into the () primarily through stellar winds and explosive outflows, respectively. In AGB stars, on newly formed grains accelerates the material to velocities of 5–20 km s⁻¹, forming expansive circumstellar envelopes that merge with the over time. explosions propel at speeds exceeding 10,000 km s⁻¹, distributing across large volumes and contributing to galactic enrichment on short timescales. These mechanisms ensure that stellar-sourced serves as the initial seed population for further processing in the . Observational evidence for dust formation in these environments comes from infrared spectroscopy, particularly the 9.7 μm absorption feature attributed to the Si–O stretching mode in amorphous silicates surrounding AGB stars. This band, prominent in spectra of oxygen-rich AGB stars, has been resolved and confirmed using the Spitzer Space Telescope's Infrared Spectrograph (IRS) and the Herschel Space Observatory's Photodetector Array Camera and Spectrometer (PACS). For supernovae, mid-infrared excesses in remnants like Cassiopeia A reveal silicate and carbon features, supporting in-situ formation models. Chemical evolution models indicate that AGB stars contribute approximately 30–50% of the interstellar budget in galaxies like the , with yields scaling with and , while Type II supernovae account for 20–30%, particularly dominant in the early . These estimates, derived from simulations incorporating efficiencies of 0.2–0.5 for refractories, highlight the complementary roles of low- and high-mass in sustaining the cosmic cycle.

Growth in Interstellar Medium

In the interstellar medium (ISM), cosmic dust grains initially ejected from stars grow through accretion of gas-phase atoms and molecules onto their surfaces, as well as coagulation where small grains collide and aggregate into larger ones, primarily driven by van der Waals forces and sticking probabilities around 0.3. These processes are most efficient in dense molecular clouds, where turbulent motions and thermal velocities facilitate collisions, leading to grain size increases at rates of approximately 10−310^{-3} μm per million years for sub-micron particles. For instance, in solar-metallicity environments, accretion can deplete small grains (<0.001 μm) within 10 million years, while coagulation further shifts the size distribution toward larger aggregates around 0.002 μm on similar timescales. Ice mantle formation significantly contributes to this growth in cold ISM regions with temperatures below 100 K and densities around 10410^4 cm⁻³, where volatile species such as H₂O (the dominant component, exceeding 60% of ice mantles) and NH₃ adsorb onto grain surfaces, forming multilayer icy coatings through physisorption and surface reactions. These mantles, primarily water-dominated, can increase the effective grain radius by 20-50% by adding substantial mass via successive monolayer buildup, with H₂O molecules binding more strongly on silicate surfaces than carbon ones. This process not only enlarges grains but also enables catalytic chemistry, enhancing the overall dust population in molecular clouds. Destruction mechanisms counteract growth, recycling dust through sputtering in interstellar shocks (removing 10-20% of silicate material per crossing at velocities of 50-150 km s⁻¹), UV photolysis that dehydrogenates carbonaceous grains in diffuse regions, and cosmic ray erosion that amorphizes crystalline components over longer timescales. These processes maintain a balance, with dust lifetimes around 200-400 million years, ensuring continuous replenishment from stellar sources while limiting net accumulation. Models of dust evolution adopt a two-phase paradigm, starting with stardust seeds from stellar ejecta that subsequently grow in the ISM via accretion and coagulation, with grain radius evolution described by equations such as a˙=ξ(t)a/τ(a)\dot{a} = \xi(t) a / \tau(a), where τ(a)\tau(a) scales inversely with gas density ρgas\rho_\mathrm{gas}, sticking efficiency, and relative velocity vrelv_\mathrm{rel}, leading to mass enhancements of 18-33% for graphite and silicates over 10-30 million years in dense clouds. Recent simulations, informed by James Webb Space Telescope (JWST) observations between 2022 and 2025, confirm this hybrid growth in molecular clouds, highlighting efficient ISM accretion as a key pathway for hydrocarbon grain formation alongside stellar origins.

Detection and Observation

Remote Sensing Methods

Remote sensing methods enable astronomers to detect and characterize cosmic dust across vast distances by analyzing its interactions with electromagnetic radiation, without direct physical contact. These techniques span multiple wavelengths, from ultraviolet to radio, leveraging the dust's absorption, scattering, and emission properties to map distributions, infer compositions, and study dynamics in interstellar and intergalactic environments. Infrared observations, in particular, are crucial for penetrating obscuring dust layers and revealing emission from heated grains. Infrared telescopes like the , operational from 2003 to 2020, have extensively mapped cosmic dust emission by detecting thermal radiation from dust grains warmed by starlight. instruments, including the Infrared Array Camera and Multiband Imaging Photometer, resolved dust structures in nearby galaxies and the Milky Way, identifying features such as extended dust disks and obscured star-forming regions. The (), launched in 2021, builds on this with superior sensitivity and resolution, achieving angular scales of approximately 0.1 arcseconds to map dust emission in unprecedented detail, such as intricate networks of gas and dust in star-forming galaxies like NGC 628. Optical and ultraviolet extinction measurements quantify cosmic dust by observing the dimming and reddening of starlight passing through dusty regions. The visual extinction AVA_V is proportional to the line-of-sight integral of dust number density ndn_d and extinction cross-section σext\sigma_{\rm ext}, given by AV∝∫ndσext dlA_V \propto \int n_d \sigma_{\rm ext} \, dl, where the factor of proportionality relates to the optical depth via magnitudes. Surveys like the Gaia mission, ongoing since 2013, utilize precise stellar photometry and parallaxes to construct three-dimensional dust maps across the , revealing extinction variations with distance and revealing clumpy structures in the interstellar medium. Polarimetry detects aligned dust grains by measuring the polarization of scattered or transmitted starlight, which arises from non-spherical grains oriented by magnetic fields or radiation in the interstellar medium. In diffuse regions, polarization levels typically range from 1% to 10%, providing insights into grain shapes, sizes, and alignment mechanisms, such as radiative torques on silicate-dominated grains. Observations from ground-based and space telescopes, including those targeting Mg, Si, and Fe abundances in sightlines, confirm that silicate grains are primary polarizers, with polarization efficiency tied to elemental depletions. At radio and sub-millimeter wavelengths, facilities like the Atacama Large Millimeter/submillimeter Array (ALMA) observe cold cosmic dust (temperatures around 20 K) through its thermal continuum emission, which traces mass and distribution in molecular clouds and distant galaxies. ALMA's high-resolution imaging, such as in NGC 628 at 0.87 mm and 2.1 mm bands, reveals compact sources associated with star clusters, with emission slopes indicating grain properties. These observations complement shorter wavelengths by probing the coldest phases unaffected by stellar heating. Recent advances with JWST's Mid-Infrared Instrument (MIRI), utilizing data from 2022 onward, have unveiled in early at redshifts z>10z > 10, approximately 400 million years after the . MIRI's , as in the case of the GHZ2 at z=12.33z = 12.33, detects emission lines amid dusty environments, inferring low metallicities and high rates in obscured systems, challenging models of rapid dust production in the young universe, complemented by 2025 ALMA observations confirming extreme .

In-Situ Measurements and Sample Returns

In-situ measurements of cosmic dust have provided direct insights into its composition and dynamics through spacecraft instruments and returned samples, enabling laboratory analyses that reveal micro-scale properties unattainable by remote methods. The Stardust mission, launched in 1999 and returning samples in 2006, collected dust from the coma of comet 81P/Wild 2 using collectors, yielding a total sample mass of approximately 1 mg comprising thousands of particles ranging from nanometers to micrometers in size. These particles exhibited diverse morphologies, including and organic compounds, confirming the comet's role as a presolar material reservoir. Subsequent missions expanded this approach to asteroids. Japan's Hayabusa2 spacecraft, operating from 2014 to 2020, returned 5.4 grams of material from the C-type asteroid Ryugu, including organic-rich particles such as aromatic hydrocarbons and amino acid precursors captured via touch-and-go sampling. Initial analyses highlighted the samples' primitive nature, with soluble organics indicating aqueous alteration on the asteroid. NASA's OSIRIS-REx mission, which delivered samples from asteroid Bennu in 2023, returned over 120 grams of regolith dominated by hydrated silicates like phyllosilicates, alongside sulfides, magnetite, and carbon-rich matter; analyses as of 2025 reveal 14 of 20 amino acids found in Earth biology and all five nucleobases in DNA and RNA, underscoring Bennu's history of water-rock interactions. For interstellar dust, in-situ detectors on missions like Ulysses (1990–2009) and Cassini's Cosmic Dust Analyzer (CDA, 1997–2017) measured particle fluxes and trajectories, identifying grains with inflow velocities exceeding 20 km/s, peaking near 26 km/s relative to the Sun. These instruments detected dozens of interstellar particles annually, distinguishing them from solar system dust by their hyperbolic orbits and compositions rich in silicates and organics. Laboratory analyses of returned samples employ high-resolution imaging and spectroscopic techniques to characterize morphology and isotopic signatures. Scanning electron microscopy (SEM) and (TEM) reveal particle structures, such as fractal aggregates in Wild 2 dust and layered phyllosilicates in material. , including secondary ion mass spectrometry (SIMS) and gas-source isotope ratio mass spectrometry, identifies isotopic anomalies like ¹⁵N enrichments (up to δ¹⁵N = +266‰) in Stardust organics, pointing to interstellar origins. These methods preserve sample integrity while quantifying trace elements and molecular species. Key challenges in these efforts include minimizing terrestrial contamination and optimizing capture media. , used in Stardust to decelerate particles while preserving about 10,000 tracks, suffered from manufacturing contaminants like silica and organics, requiring rigorous subtraction during analysis. Strict protocols, such as cleanroom handling and witness plate monitoring, are essential for missions like to ensure sample purity, as even trace volatiles could obscure primordial signatures.

Interactions with Radiation

Absorption and Scattering

Cosmic dust grains interact with primarily through absorption and processes, which together constitute —the removal of photons from the beam of incoming . The total cross-section for a single grain is given by σext=σabs+σsca\sigma_\mathrm{ext} = \sigma_\mathrm{abs} + \sigma_\mathrm{sca}, where σabs\sigma_\mathrm{abs} is the absorption cross-section and σsca\sigma_\mathrm{sca} is the cross-section. For spherical grains, these cross-sections are calculated using Mie theory, which provides exact solutions for the interaction of plane waves with homogeneous spheres; in the limit where the grain radius aa is much smaller than the λ\lambda (Rayleigh regime), the efficiency QextQ_\mathrm{ext} approximates Qext∝2πa/λQ_\mathrm{ext} \propto 2\pi a / \lambda. The wavelength dependence of these interactions leads to preferential scattering of shorter wavelengths, such as blue light, over longer ones in the Rayleigh regime, resulting in the observed reddening of passing through dusty regions. This interstellar reddening is quantified by the total-to-selective ratio RV=AV/E(B−V)≈3.1R_V = A_V / E(B-V) \approx 3.1, the standard value for the diffuse in the , where AVA_V is the visual and E(B−V)E(B-V) is the color excess in the BB and VV bands. Non-spherical grain shapes and distributions further modulate this , but the RV≈3.1R_V \approx 3.1 captures the average behavior across many sightlines. Dust grains often align with the local , influencing patterns and producing observable effects like of transmitted light. In the Davis-Greenstein mechanism, paramagnetic relaxation aligns the short axes of grains perpendicular to the lines, leading to dichroic absorption and that polarize background along the field direction. This alignment is particularly effective for suprathermal rotation induced by radiative torques, enhancing polarization signals at optical and wavelengths. Absorption of heats individual grains to an equilibrium TT where the power absorbed from the interstellar field balances the power re-emitted thermally. For typical diffuse medium conditions, this yields grain temperatures of 15–20 K for silicates and slightly higher for graphites, depending on and composition. These heated grains subsequently emit in the , as detailed in related studies on signatures. Observationally, absorption and by cosmic dust significantly obscure and optical light, with estimates indicating that approximately 50% of such emission from star-forming regions in galaxies is extinguished along typical lines of sight. This not only reddens spectra but also requires corrections in estimates, affecting our understanding of galaxy evolution and rates. In dense environments, the effect is even more pronounced, rendering entire regions optically thick.

Thermal Emission and Spectral Signatures

Cosmic dust grains absorb interstellar radiation and re-emit the energy primarily as thermal emission in the and submillimeter wavelengths. This process follows a modified blackbody , where the intensity is given by Iν=ϵνBν(T)I_\nu = \epsilon_\nu B_\nu(T), with Bν(T)B_\nu(T) representing the Planck blackbody function at TT and ϵν\epsilon_\nu the frequency-dependent . For small grains, ϵν∝ν2\epsilon_\nu \propto \nu^2, reflecting their efficient emission at longer wavelengths due to the Rayleigh-Jeans tail of the blackbody curve. Characteristic spectral features in the thermal emission provide diagnostics of dust composition. The 10 μ\mum stretching mode appears as a broad emission or absorption band from amorphous silicates, while the 3.3 μ\mum (PAH) C-H band arises from vibrational modes in aromatic carbon structures. Additionally, the 2175 Å bump is attributed to π→π∗\pi \to \pi^* electronic transitions in graphitic or PAH components, influencing the overall . In protoplanetary disks, dust temperatures exhibit radial gradients due to varying stellar heating, with inner regions reaching 50–100 and outer regions cooling to 10–20 . These gradients shape the emission profiles, enabling mapping of disk through multi-wavelength observations. Dust emission spectra are modeled by combining grain size distributions, compositions, and temperatures to fit observations. The Draine-Li model (2007), incorporating silicates, , and PAHs, reproduces emission and extinction, with updates in the 2020s, such as the Astrodust+PAH model incorporating composite "astrodust" grains to describe dust properties. These models facilitate compositional inferences from spectral fitting. Recent (JWST) observations have resolved thermal dust emission in protostars, revealing asymmetric distributions in collapsing envelopes and disks from 2023–2025 data. JWST has enabled detection of dust emission in galaxies at z > 10, constraining early dust production (as of 2025).

Astrophysical and Astrobiological Roles

Influence on Star and Planet Formation

Cosmic dust plays a pivotal role in the of molecular clouds by facilitating , which enables fragmentation into multiple substructures that seed . At low densities, gas cooling is dominated by molecular line emission, but as densities approach the critical value of approximately 10−2010^{-20} g/cm³ (corresponding to number densities n∼104n \sim 10^4 cm⁻³), dust grains become the primary coolant through thermal infrared emission. This dust-mediated cooling reduces the temperature and sound speed in collapsing regions, lowering the Jeans mass and allowing the cloud to fragment into smaller cores rather than forming a single massive star. Simulations demonstrate that without dust cooling, fragmentation is suppressed, leading to higher-mass star formation, whereas dust enables the production of low-mass fragments essential for a realistic . Dust also influences star and planet formation through its opacity, which shields dense regions from ultraviolet (UV) radiation and promotes molecular hydrogen (H₂) formation. Interstellar dust grains absorb and scatter UV photons from nearby stars, creating shadowed zones where H₂ can form on grain surfaces via recombination of atomic hydrogen without immediate photodissociation. This shielding is crucial in star-forming regions, where dust opacity reduces the UV flux, enabling H₂ self-shielding and the transition to molecular gas necessary for further collapse. In protoplanetary disks (PPDs), dust opacity regulates the temperature profile, contributing to disk stability by preventing excessive heating and supporting the formation of long-lived structures conducive to planet growth. A key mechanism for planetesimal formation involves the in PPDs, where dust particles concentrate into dense clumps under aerodynamic interactions with the gas. In the Youdin-Goodman model, differential drift between dust and gas in a Keplerian disk triggers this , amplifying particle concentrations when the dust-to-gas ratio exceeds unity and particles reach optimal sizes of 1-10 cm (corresponding to Stokes numbers near 0.1-1). These pebble-sized grains settle toward the midplane and form axisymmetric clumps that can gravitationally collapse into kilometer-scale , bypassing the meter-sized barrier to growth. This process is most efficient in turbulent disks with moderate , providing the building blocks for rocky planets and cores of gas giants. Observational evidence from high-resolution imaging underscores dust's role in these processes, with Atacama Large Millimeter/submillimeter Array (ALMA) observations of the HL Tauri protoplanetary disk in 2014 revealing concentric dust rings and gaps indicative of early planet formation carving pathways through the disk. More recent James Webb Space Telescope (JWST) surveys of PPDs from 2022 to 2025 have detected similar substructures, including gaps in disks like PDS 70 attributed to forming protoplanets, confirming dust concentration and dynamical interactions in real systems. Additionally, dust contributes to feedback via outflows in young stars, where radiation pressure on dust grains drives molecular outflows that regulate accretion and disperse surrounding material, limiting further star formation in clusters.

Connections to Organic Chemistry and Life Origins

Cosmic dust grains play a pivotal role in interstellar chemistry by catalyzing the formation of molecular (H₂) through surface reactions, with an observed formation rate coefficient of approximately 3–4 × 10⁻¹⁷ cm³ s⁻¹ in the diffuse (). This process involves hydrogen atoms physisorbing onto grain surfaces, diffusing, and recombining, which is essential for shielding denser regions from radiation and enabling further molecular synthesis. Additionally, icy mantles on these grains undergo driven by cosmic rays and UV photons, leading to the production of (CH₃OH) from simpler precursors like CO and H atoms, as well as intermediates that contribute to formation. Laboratory simulations confirm that such ice yields complex organics, including precursors, under conditions mimicking cold molecular clouds. Polycyclic aromatic hydrocarbons (PAHs), comprising 10–20% of the cosmic carbon budget in interstellar dust, serve as key building blocks for more complex organics. These carbon-rich molecules, often hosted on or within dust grains, can evolve through processing in the ISM and incorporation into meteorites, where they contribute to the synthesis of amino acids. Analyses of the Murchison meteorite, a carbonaceous chondrite, have identified over 70 amino acids, including non-proteinogenic ones derived from interstellar precursors, supporting the role of dust in prebiotic organic evolution. In dense regions, grain-surface reactions dominate over gas-phase pathways for forming complex organic molecules (COMs), as low temperatures favor accretion and radical recombination on icy surfaces. From an astrobiological perspective, cosmic dust has facilitated the delivery of organics to the around 4 billion years ago (Ga), providing a flux of prebiotic compounds during the . This delivery mechanism likely seeded planetary surfaces with life's building blocks, including and nucleobases preserved in meteoritic material. Recent observations in 2023 detected glycolamide (NH₂COCH₂OH), a glycine isomer, in the for the first time, highlighting ongoing in distant clouds. Furthermore, samples returned from asteroid Ryugu in 2020 revealed uracil, a key nucleobase, at concentrations of 7 ± 4 ppb and 21 ± 6 ppb, underscoring dust and small bodies as vectors for astrobiologically relevant molecules.

Distribution and Notable Examples

Interplanetary and Zodiacal Dust

Interplanetary dust, also known as the zodiacal cloud, consists of microscopic particles distributed throughout the inner Solar System, primarily between 0.2 and 5 from the Sun. These particles originate from multiple sources, including collisions among asteroids in the main belt, from comets, and ejections from the . Asteroid collisions contribute a significant of the dust through fragmentation during impacts, producing particles that are subsequently shaped by solar radiation pressures. Cometary activity, particularly from Jupiter-family comets, supplies dust via sublimation and fragmentation, with models indicating these as the dominant source for maintaining the cloud's steady state. Kuiper Belt objects provide longer-lived contributions, with dust grains transported inward over timescales of millions of years. The total mass of the zodiacal cloud is estimated at approximately 3×10163 \times 10^{16} kg, equivalent to a small , sustained by a continuous influx balanced by removal processes. The spatial distribution of interplanetary dust shows a peak density near 1 , where the mass density reaches about 10−2210^{-22} g/cm³ for micron-sized grains, decreasing radially outward due to dynamical effects. This distribution is influenced by Poynting-Robertson drag, a non-keplerian force from solar radiation and thermal emission that causes particles to spiral inward, concentrating dust in the inner Solar System. For grains with radiation pressure-to-gravity ratio β > 1—known as β-meteoroids—the drag effect is amplified, leading to hyperbolic orbits that eject smaller particles out of the plane and beyond the . The , a visible phenomenon, arises from scattered by these predominantly micron-sized grains, with following an approximate proportionality to sin⁡(ϵ)\sin(\epsilon), where ϵ\epsilon is the solar elongation angle, explaining its diffuse, cone-shaped appearance along the ecliptic. Planetary influences create localized enhancements within the broader zodiacal cloud. A circumsolar dust ring encircles ' orbit, formed by impacts and collisions involving co-orbital asteroids, producing a narrow band of particles confined by gravitational resonances. Similarly, a surrounds , originating from volcanic eruptions on Io, where silicate and sulfur-rich ejecta are lofted into the , charged by plasma interactions, and distributed azimuthally around the planet. These structures highlight how giant planets modify the interplanetary population through gravitational and electromagnetic effects. Recent in-situ measurements from the , launched in 2018 and operational through 2025, have provided unprecedented data on dust flux near the Sun, down to 0.17 AU. The probe's FIELDS and WISPR instruments detect impact rates and imaging, revealing higher-than-expected fluxes of sub-micron particles ejected radially by , with densities increasing toward perihelion and confirming the role of inner Solar System sources in replenishing the zodiacal cloud. These observations refine models of dust dynamics in the harsh near-Sun environment.

Prominent Dusty Clouds and Nebulae

are regions where interstellar scatters from nearby , often appearing blue due to the higher scattering efficiency of shorter wavelengths. A prominent example is the surrounding the young in Taurus, where grains reflect the blue from hot B-type , with scattering efficiency Q\sca≈1Q_{\sca} \approx 1 at visible wavelengths for typical grain sizes of 0.1–1 μm. This scattering reveals the three-dimensional structure of the cloud, extending several parsecs around the cluster and providing insights into local properties. Emission nebulae highlight dust's role in ionized regions powered by massive stars. The (M42), a bright in Orion, contains approximately 103 M⊙10^3 \, M_\odot of dust within its complex, which is actively forming around 1000 young stars embedded in dense filaments. Dust here absorbs ultraviolet radiation from the central Trapezium stars and re-emits in the , outlining pillars of gas and dust that serve as stellar nurseries. Another key example is the , a from the 1054 CE explosion, where dust grains—estimated at 0.03–0.05 M⊙M_\odot of —survive in the expanding shell and contribute to emission amid from the . Molecular clouds represent dense, cold reservoirs of dust and gas that foster low-mass . The Taurus-Auriga complex, a nearby filamentary cloud spanning about 100 deg², maintains a dust-to-gas of approximately 1:100, with total dust mass around 150 M⊙M_\odot supporting the formation of hundreds of solar-type stars over several million years. Dust extinction maps reveal substructures like dense cores (e.g., Barnard 18) where grains shield molecular , enabling collapse under gravity. On galactic scales, cosmic dust concentrates in spiral arms, forming prominent dust lanes that trace (ISM) density waves. In the , these lanes enrich the arms with silicates and carbonaceous grains, comprising about 1% of the ISM's total mass and obscuring background stars in visible light while emitting thermally in the . Observations show dust lanes aligning with molecular gas concentrations, such as in the Perseus Arm, where they fuel ongoing bursts. Extragalactic examples extend these features to other galaxies. In the (M31), dark dust lanes wind through the spiral arms, revealed by imaging that penetrates the obscuration to show concentrations of cold dust near star-forming regions. Recent (JWST) observations of high-redshift (z ≈ 6) quasars have uncovered dusty host galaxies, where obscured supermassive black holes are enveloped in dense dust tori and extended disks, bridging luminous unobscured quasars and their progenitors during . As of 2025, JWST data also indicate inefficient dust production in massive, metal-rich galaxies at z=7.13 and varied dust attenuation trends across z ∼ 2–11.5, highlighting rapid dust enrichment in the early . These views highlight dust's ubiquity in early galaxy , with emission from polycyclic aromatic hydrocarbons and silicates indicating rapid enrichment.

Delivery to Earth and Terrestrial Impacts

Pathways from Space to Earth

Cosmic dust reaches primarily through the influx of micrometeorites, with an estimated annual accretion of to tonnes, predominantly particles smaller than 100 μm in diameter. Approximately 90% of this material ablates during due to intense heating and friction, leaving about 10% to survive as micrometeorites that settle to the surface. The total daily influx is around 43 tonnes, with contributions varying by source and particle size. The vast majority—over 99%—of this originates from interplanetary sources within the solar system, including Jupiter-family comets (contributing about 80%), asteroids (around 8%), and long-period comets (roughly 12%). Less than 1% consists of interstellar dust, with only seven particles confirmed as extrasolar by the Stardust mission through their anomalous compositions and trajectories. Particles from Jupiter-family comets dominate the zodiacal cloud and thus the influx, entering Earth's atmosphere on hyperbolic trajectories relative to the planet at velocities typically between 12 and 15 km/s, decelerating rapidly beginning at altitudes of about 100 km due to aerodynamic drag. Larger particles experience entry speeds up to 50 km/s from long-period sources, intensifying frictional heating. During entry, depends on , , and composition; particles larger than 100 μm often partially or fully melt, forming cosmic spherules such as iron-rich (I-type), glassy (G-type), or stony (S-type) varieties due to temperatures exceeding 1,500 K at 10–50 km/s impacts. Pristine, unmelted particles—retaining original textures and organics—predominantly include those smaller than 10 μm, which decelerate with minimal heating and experience less than 1% mass loss. Partially melted scoriaceous forms represent transitional , with overall reducing the influx to 5,200 tonnes per year of surviving material, as quantified from collections. Deposition exhibits seasonal variations driven by orbital dynamics and meteor showers; for instance, the Perseid shower in August elevates flux from comet 109P/Swift-Tuttle dust trails, increasing input by factors of 10–100 during peaks. In polar regions like , accumulation is enhanced by snow, which traps and preserves particles with minimal terrestrial contamination, leading to higher measured fluxes (e.g., 5200 tonnes/year at Dome C) compared to global averages. These variations underscore the role of sporadic sources in modulating delivery, with latitude-dependent patterns observed in radar data.

Collection, Analysis, and Environmental Effects

Cosmic dust particles that survive to reach Earth's surface are collected from diverse terrestrial archives, providing insights into their flux and composition. In polar regions, ice cores from sites such as 's Dome C and Greenland's preserve micrometeorites and cosmic spherules in layered ice, enabling reconstruction of historical deposition rates over millennia. Deep-sea sediments serve as another key repository, where techniques extract cosmic spherules from ocean floor deposits, as demonstrated in collections from the Central Basin yielding over 1,200 particles. Urban environments have emerged as accessible collection sites, with rooftop filters capturing micrometeorites amid anthropogenic debris; a 2017 study recovered more than 500 large micrometeorites (>100 μm) from rooftops, highlighting variations in extraterrestrial dust flux. expeditions spanning the 1980s to 2020s have been particularly productive, with efforts like those at the and yielding thousands of particles—over 100,000 large interplanetary dust particles (>50 μm) from processed alone—while recent 2020s urban melt collections in and snow sieving near stations have added over 1,000 additional micrometeorites. As of 2025, the cumulative number of micrometeorites retrieved from urban collections exceeds that of reference collections, with individual efforts such as Larsen's totaling nearly 6,000 samples. Once collected, these particles undergo detailed analysis to characterize their structure, composition, and origins. Micro-computed tomography (μ-CT) reveals three-dimensional internal textures, such as porous structures or mineral inclusions in unmelted micrometeorites, without destructive sampling. Secondary ion mass spectrometry (SIMS) measures isotopic ratios, particularly oxygen isotopes (δ¹⁷O and δ¹⁸O), to infer formation environments and parent bodies. Distinguishing cosmic dust from terrestrial contaminants relies on elemental ratios; for instance, cosmic particles typically exhibit Ni/Fe ratios around 0.05, higher than the crustal average of ~0.002, while Fe/Ni and Fe/Cr ratios further aid classification, as seen in microspherules from sediments. Isotopic tracing addresses key gaps in provenance, linking particles to specific sources like comets through anomalous ¹⁶O-depleted compositions matching those in comet 81P/Wild 2 samples. The environmental impacts of Earth-fallen cosmic dust are subtle but noteworthy. Approximately 5,200 metric tons of micrometeorites reach the surface annually, a flux dominated by particles under 100 μm that largely survive atmospheric heating. This material contributes trace elements such as iron, , and to soils, acting as a for ecosystems, particularly in nutrient-poor regions like glacial environments where it may have enhanced prebiotic chemistry. Despite containing cosmogenic radionuclides like ²⁶Al, the dispersed low mass poses no significant hazard to terrestrial or human health.

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