Space dust measurement
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Ever since the beginning of the space age satellites and space probes performed space dust measurements. The goal was, initially, to quantify the hazard of meteoroid impacts onto space vehicles. Samples returned to Earth by the Apollo astronauts demonstrated that the lunar surface is peppered by microcraters generated by high speed impacts of cosmic dust particles. Their analysis provided a measurement of the flux of interplanetary dust particles. The later goal of dust measurements was the exploration of the dust environments throughout interplanetary space, within planetary systems, and, today, it is to analyze planetary bodies from which dust particles originate. The development of instrument swent from simple and small but noisy microphone detectors, over large and reliable multi-coincidence dust detectors to sophisticated dust analyzers that determine the composition of individual dust particles.
Overview
From the ground space dust is observed as scattered sun light from myriads of interplanetary dust particles and as meteoroids entering the atmosphere. By observing a meteor from several positions on the ground the trajectory and the entry speed can be determined by triangulation. Atmospheric entry speeds of up to 72,000 m/s have been observed for Leonid meteors. It was obvious that even sub-millimeter sized meteoroids hitting a spacecraft at speeds much faster than bullets at ~300 m/s can cause significant damage. Therefore, the early US Explorer 1, Vanguard 1 and the Soviet Sputnik 3 satellites carried simple 0.001 m2 sized microphone dust detectors in order to detect impacts of micron sized meteoroids.[1][2][3] The obtained fluxes were orders of magnitude higher than those estimated from zodiacal light measurements.[4] However, the latter determination had big uncertainties in the assumed size and heliocentric radial dust density distributions. Thermal studies in the lab with microphone detectors [5] suggested that the high count rates recorded were due to noise generated by temperature variations in Earth orbit. An excellent review of the early days of space dust research was given by Fechtig, H., Leinert, Ch., and Berg, O.[6] in the book Interplanetary Dust.[7]
Dust accelerators
A critical facility to develop, test, and calibrate space dust instruments is a dust accelerator.[8] Classic guns have muzzle velocities of a few 100 m/s to about 1 km/s whereas meteoroid speeds range from a few km/s to several 100 km/s for nanometer sized dust particles. Only experimental light-gas guns (e.g. at NASA's Johnson Space Center, JSC[9]) reach projectile speeds of several km/s up to 10 km/s in the laboratory. By exchanging the projectile with a sabot[10] containing any dust particles high speed dust projectiles can be used for impact cratering and dust sensor calibration experiments. The workhorse for hypervelocity dust impact experiments is the electrostatic dust accelerator.[11] Nanometer to micrometer sized conducting dust particles are electrically are charged and accelerated by an electrostatic particle accelerator to speeds up to 100 km/s. Currently operational dust accelerators exist at IRS[12] in Stuttgart, Germany (formally at Max Planck Institute for Nuclear Physics in Heidelberg[13]) and at Laboratory for Atmospheric and Space Physics (LASP) in Boulder, Colorado.[14] The LASP dust accelerator facility is operational since 2011, and has been used for basic impact studies, as well as for the development of dust instruments. The facility is available for the planetary and space science communities.[15] Dust accelerators are used for impact cratering studies,[16] calibration of impact ionization dust detectors,[17] and meteor studies.[18] Only electrically conducting particles can be used in an electrostatic dust accelerator because the dust source is located in the high-voltage terminal. James F. Vedder,[19] at Ames Research Center, ARC, used a linear particle accelerator by charging dust particles by an ion beam in a quadrupole ion trap under visual control. This way a wide range of dust materials could be accelerated to high speeds.[20]
Reliable dust detections
Tennis court sized (200 m2) penetration detectors on the Pegasus satellites[21] determined a much lower flux of 100 micron sized particles that would not pose a significant hazard to the manned Apollo missions. First reliable dust detections of micron-sized meteoroids were obtained by the dust detectors on board the Pioneer 8/9[22] and HEOS 2[23] spacecraft. Both instruments were impact ionization detectors using coincident signals from ions and electrons released upon impact. The detectors had sensitive areas of ~0.01 m2 and detected outside the Earth's magnetosphere on average one impact per ten days.
Microcrater analyses
Microcraters on lunar samples (Figure 1) provide an extensive record of impacts onto the lunar surface. Uneroded glass splashes from big impacts covering crystalline lunar rocks preserve well microcraters. Microscopic and scanning electron microscopic analyses[24][25] result in microcrater densities on a single sample of craters with diameters ranging from 10−8 to 10−3 m. Impact crater sizes were related to meteoroid masses based on dust accelerator simulations[26] assuming an effective impact speed onto the lunar surface of 20 km/s. Since no reliable surface exposure age could be determined from solar flare track densities on the same rocks spacecraft measurements were used to determine the interplanetary dust flux at 1 AU[27] (Figure 2). The crater production flux at 100 μm size (~ 10 m−9 kg) was adjusted to the flux observed by the Pegasus satellites. The flux of micron sized and smaller meteoroids is smaller than the respective cratering flux on the lunar surface because of the significant fast ejecta flux from nearby impacts of bigger meteoroids. This flux was adjusted to the meteoroid flux observed by the HEOS-2 and Pioneer 8/9 space probes.
For 5.7 years from April 1984 to January 1990 the NASA's Long Duration Exposure Facility exposed several passive impact collectors of several square meters area to the space dust environment in low Earth orbit. After recovery of LDEF by Space Shuttle Columbia the instrument trays were returned to and analyzed by the investigators. The results[28][29] generally confirmed the earlier analysis of lunar microcaters.[27]
Optical and infrared zodiacal dust observations
Zodiacal light observations at different heliocentric distances were performed by the Zodiacal light photometer instruments on Helios 1 and 2[30] and the Pioneer 10 and 11[31] space probes between 0.3 AU and 3.3 AU from the sun. This way the heliocentric radial profile was determined which varied by a factor approx. 100 over that distance. The Asteroid Meteoroid Detector, AMD,[32] on Pioneer 10 and 11 used the optical detection and triangulation of individual meteoroids to get information on their sizes and trajectories. Unfortunately, the trigger threshold was set too low that noise corrupted the data.[33] Zodiacal light observations at visible light wavelengths use the light scattered by interplanetary dust particles which is only a few percent of the incoming light. The remainder of ca. 90% is absorbed and reradiated at infrared (IR) wavelengths.
The IR brightness of the Zodiacal dust cloud is much stronger than the brightness at visible wavelengths and dominates the sky brightness. However, on the ground most of the thermal IR sky brightness is blocked by atmospheric absorption bands, therefore, most of IR astronomy observations are done from space observatory satellites. The Infrared Astronomical Satellite, IRAS, mapped the sky at 12, 25, 60 and 100 micrometers wavelength. At 12 to 60 microns wavelengths zodiacal dust was a prominent feature. Later the Diffuse Infrared Background Experiment, DIRBE, on NASA's COBE mission provided a complete high precision survey of the Zodiacal dust cloud[34] at the same wavelengths.[35]
Already IRAS infrared sky maps showed structure in the sky brightness. Within the wide general Zodiacal cloud and a broad central asteroidal band there were several narrow cometary trails.[36] Follow-up observations using the Spitzer Space Telescope showed that at least 80% of all Jupiter family comets had trails.[37] When the Earth passes through a comet trail a meteor stream is observed form the ground. Because the enhanced risk to spacecraft in such meteoroid streams ESA developed the IMEX model[38] which followed the evolution of cometary particles[39] and hence allows us to determine the risk at specific positions and times in the inner solar system.
Penetration detectors
In the early 1960th engineering type pressurized cell micrometeorite detectors were flown on the Explorer 16 and Explorer 23 satellites. Each satellite carried more than 200 individual gas filled pressurized cells of 25 and 50 micron metal wall thickness. A puncture of a cell by a meteoroid impact was detected by a pressure sensor. These instruments provided important measurements of the near Earth meteoroid flux.[40] In 1972 and 1973 the Pioneer 10 and 11 interplanetary spacecraft carried 234 pressurized cell detectors each mounted on the back of the main dish antenna. The stainless steel wall thickness was 25 micron on Pioneer 10, and 50 micron on Pioneer 11. The two instruments characterized the meteoroid environment in the outer solar system as well as near Jupiter and near Saturn.[41]
In preparation of the Apollo Missions to the moon three Pegasus satellites were launched by the Saturn 1 rocket into near Earth orbit. Each satellite carried 416 individual meteoroid detectors totaling approx. 200 m2 detection surface. The detectors consisted of 171 m2 of 400 micron, 16 m2 of 200 micron, and 7.5 m2 of 40 micron thick aluminum penetration sheets. Placed behind the penetration sheets were 12 micron thick mylar capacitor detectors that recorded penetrations of the overlying sheet.[42] The results showed that the meteoroid hazard is significant and meteoroid protection methods must be implemented for large space vehicles.[40]
In 1986 John Simpson flew on the Vega 1 and 2 missions a new dust detector using polyvinylidene difluoride PVDF films.[43] This material responds to dust impacts by generating electrical charge due to impact cratering or penetration.[44] Since PVDF detectors are also sensitive to mechanical vibrations and energetic particles, detectors using PVDF work acceptably well as High rate dust detectors, HRD, in high dust density dust environments like in cometary comae or on the Cassini Cosmic Dust Analyzer in planetary rings.[45] The Dust Flux Monitor Instrument, DFMI, on the Stardust mission used also PVDF detectors to study dust in the coma of comet Wild 2. In interplanetary space, however, the PVDF detectors on the Venetia Burney Student Dust Counter needed reference detectors which are shielded from dust impacts in order to determine the background noise rate.[46]
Modern microphone detectors
A 1 mm thick front shield (Whipple shield of 1.85 m diameter) together with the 12 mm thick Kevlar rear shield protected the Giotto spacecraft from dust from Halley's Comet during its flyby at 600 km distance. Mounted on the front dust shield were three piezoelectric momentum sensor of the Dust Impact Detection System, DIDSY.[47] A fourth momentum sensor was mounted on the rear sheet. These microphone detectors together with other detectors measured the dust distribution within the inner coma of comet 1P/Halley.[48] This instrument measured also dust during Giotto encounter with comet 26P/Grigg–Skjellerup.[49]
On the Mercury Magnetospheric Orbiter[50] of the BepiColombo mission the Mercury Dust Monitor (MDM)[51] will measure the interplanetary and Mercury dust environments.[52] MDM is composed of four piezoelectric ceramic sensors made of lead zirconate titanate, PZT. Waveforms of the impact signals will be recorded and analyzed.
Chance dust detectors
Most instruments on a spacecraft flying through a dense dust environment will see some effects of dust impacts. A prominent example of such an instrument was the Plasma Wave Subsystem, PWS, on Voyager 1 and 2 spacecraft. PWS provided useful information on the local dust environment. Initially, the Asteroid Meteoroid Detector, AMD, previously flown on Pioneer 10 and 11 was preliminarily selected for the Voyager payload. However, because there were doubts about its performance[33] the instrument was deselected and, hence, no dedicated dust instrument was carried bý the Voyager 1 and 2 spacecraft.
During the Voyager 2 flythrough through of the Saturn system PWS detected intense impulsive noise centered on the ring plane at 2.88 Saturn radii distance, slightly outside of the G ring.[53] This noise was attributed to small micron-sized particles hitting the spacecraft. In situ dust detections by the Cassini Cosmic Dust Analyzer[54] and camera observations of the outer rings confirmed the existence of an extended G ring. Also during Voyager's flybys of Uranus and Neptune dust concentrations in the equatorial planes were observed.[55][56] During the flyby of comet 21P/Giacobini-Zinner by the ICE spacecraft dust impacts were observed by the plasma wave instrument.[57] In the meantime plasma wave instruments on various spacecraft claimed the detection of dust but only in 2021 a model for the generation of signals on plasma wave antennas by dust impacts was presented based on dust accelerator tests.[58]
Impact ionization detectors
Impact ionization detectors are the most successful dust detectors in space. With help of these detectors the interplanetary dust environment from Venus to Jupiter was explored. Impact ionization detectors use the simultaneous detection of positive ions and electrons upon dust impact on a solid target. This coincidence provides a means to discriminate from noise signals on a single channel. The first successful dust detector in interplanetary space at ~ 1AU was flown on the Pioneer 8 and 9 space probes.[59] The Pioneer 8 and 9 detectors had sensitive target areas of 0.01 m2. Besides interplanetary dust on eccentric orbits it detected dust on hyperbolic orbits leaving the planetary system.[60] The HEOS 2 dust detector[61] was the first detector that employed a hemispherical geometry like all the following Galileo, Ulysses, and LDEX detectors on the LADEE mission. The hemispherical target of 0.01 m2 area collected electrons from the impact and the ions were collected by the central ion collector. These signals served to determine the mass and speed of the impacted meteoroid. The HEOS 2 dust detector explored the Earth dust environment within 10 Earth radii.[62]
The Galileo and Ulysses Dust Detectors were optimized for outer planet system dust measurements. The twin instruments were optimized for interplanetary dust measurements in the outer planetary system. The sensitive target areas were 10 fold increased to 0.1 m2 in order to cope with the expected low dust fluxes. In order to provide reliable dust impact data even within the harsh Jovian environment an electron channeltron was added in the center of the ion grid collector. This way an impact was detected by triple coincidence of three charge signals. The 2.5 tons Galileo spacecraft was launched in 1989 and cruised for 6 years interplanetary space between Venus’ and Jupiter's orbit and measured interplanetary dust.[63] The 370 kg Ulysses spacecraft was launched a year later and went on a direct trajectory to Jupiter which it reached in 1992 for a swing-by maneuver which put the spacecraft on a heliocentric orbit of 80 degrees inclination. In 1995 Galieo started its 7-year path through the Jovian system with several fly-bys of all Galilean moons. After Jupiter fly-by Ulysses identified a flow of interstellar dust sweeping through the Solar System and hyper-velocity streams of nano-dust [64] which are emitted from Jupiter and then couple to the solar magnetic field. In addition the Galileo instrument detected ejecta clounds around the Galilean moons.[65]
The Lunar Dust Experiment (LDEX)[66] on board the Lunar Atmosphere and Dust Environment Explorer (LADEE) Mission is a smaller version of the Galileo and Ulysses dust detectors. The most sensitive impact charge detector is a microchannel plate (MCP) behind the central focusing grid. LDEX has a sensitive area of 0.012 m2. The objective of the instrument was the detection and analysis of the lunar dust environment. From 16 October 2013 to 18 April 2014 LDEX detected about 140 000 dust hits at an altitude of 20 to 100 km above the lunar surface. It found a tenuous and permanent, asymmetric ejecta cloud around the Moon that is caused by meteoroid impacts onto the lunar surface.[67] From this data it was found that approximately 40 μm/Myr of lunar regolith is redistributed due to meteoritic bombardment.[68] Besides a continuous meteoroid bombardment meteoroid streams cause temporary enhancements of the ejecta cloud[69]
Dust composition analyzers
The Helios Micrometeoroid Analyzer was the in situ instrument to analyze the composition of cosmic dust. In 1974 the instrument was carried by the Helios spacecraft inside the Earth's orbit down to 0.3 AU from the sun. The goal of the Micrometeoroid Analyzer was to determine the spatial distribution of the dust in the inner planetary system, and to search for variations of the compositional and physical properties of micrometeoroids.[70] The instrument consisted of two impact ionization time-of-flight mass spectrometers (Ecliptic and South sensor) of total ~0.01 m2 target area. One sensor was shielded by the spacecraft rim from direct sun light, whereas the other sensor was protected by a thin aluminized parylene film from intense solar radiation. The Helios micrometeoroid analyzers were calibrated with a wide range of materials[71] at the dust accelerators of the Max Planck Institute for Nuclear Physics in Heidelberg and of the Ames Research Center, ARC, in Moffet Field. The mass resolution of the mass spectra of the Helios sensors was low ~ 10. There was an excess of impacts recorded by the South sensor over the impacts on the Ecliptic sensor. On the basis of the penetration studies with the Helios film[72] this excess was interpreted to be due to low density, < 1000 kg/m3 meteoroids that were shielded from entering the Ecliptic sensor.[73] Helios mass spectra range from those with dominant low masses up to 30 u that are compatible with silicates to those with dominant high masses between 50 and 60 u of iron and molecular ion types. Meteoroid streams [74] and even interstellar dust[75] particles were identified in the data.
Twin dust mass analyzers were flown on the 1986 comet Halley missions Vega 1, Vega 2, and Giotto. The spacecraft flew by Halleys comet at 600 to 10,00 km distance at 70 to 80 km/s. The twin PUMA (Vega) and PIA (Giotto) instruments were developed by Jochen Kissel of the Max Planck Institute for Nuclear Physics in Heidelberg. Dust particle hitting the small (~ 5 cm2) impact target generated ions by impact ionization. The instruments were high mass resolution (R ~ 100) reflectron type time-of-flight mass spectrometers. The instruments could record up to 500 impacts per second.[76] During Halley fly bys the instruments recorded and abundance of small (<10−14 g) particles. Besides unequilibrated silicates many of the particles were rich in light elements such as H, C, N and O.[77][78][79] This suggests that most particles consisted of a predominantly chondritic core with an refractory organic mantle.[80]
The Cometary and Interstellar Dust Analyzer (CIDA) was flown on the Stardust mission. In January 2004 Stardust flew by comet comet Wild 2 in a distance of 240 km at a relative speed of 6.1 km/s. In February 2011 Stardust flew by comet Tempel 1 in a distance of 181 km at a speed of 10.9 km/s. During interplanetary cruise between the comet encounters there were favorable phases to analyze the interstellar dust stream that was earlier discovered by the Ulysses space probe.[64] CIDA is a derivative of the impact ionization mass spectrometers flown on the Giotto and Vega 1 and Vega 2 missions. The impact target is peeking out to the side of the spacecraft while the main part of the instrument is protected from high speed dust. It has a sensitive area ~100 cm2 and a mass resolution R ~ 250. Besides the positive ion mode CIDA has also a negative ion mode for better sensitivity for organic molecules.[81] The 75 spectra obtained during the comet flybys[82] indicate a dominance of organic matter; also sulfur ions were detected in one spectrum. In the 45 spectra obtained during the cruise phase favorable for detection of interstellar particles, derivates of quinone were suggested as constituents of the organic component.[83]
The Cosmic Dust Analyzer (CDA) was flown on the Cassini mission to Saturn. CDA is a large-area (0.1 m2 total sensitive area) multi-sensor dust instrument that includes a 0.01 m2 medium resolution (R = 20 to 50) chemical dust analyzer, a 0.09 m2 highly reliable impact ionization detector, and two high rate polarized polyvinylidene fluoride (PVDF) detectors with sensitive areas of 0.005 m2 and 0.001 m2, respectively .[84] During its 6-year cruise to Saturn CDA analysed interplanetary dust,[85] the stream of interstellar dust,[86] and Jupiter dust streams.[87] A highlight was the detection of electrical dust charges in interplanetary space and in Saturn's magnetosphere [88][89] During the following 13 years Cassini completed 292 orbits around Saturn (2004 to 2017) and measured several million dust impacts that characterize dust mostly in Saturn's E ring .[90][91] In 2005 during Cassini's close flyby of Enceladus within 175 km from the surface CDA discovered active ice geysers .[92] Detailed compositional analyses found salt-rich water ice grains close to Enceladus that led to the discovery of large reservoirs of liquid water oceans below the icy crust of Enceladus.[93] Analyses of interstellar grains at Saturn's distance suggest magnesium-rich grains of silicate and oxide composition, some with iron inclusions [94]
Dust Telescopes
A Dust Telescope is an instrument to perform Dust Astronomy that not only analyses the signals and ions that are generated by a dust impact on the sensitive target but also determines the dust trajectory prior to the impact.[95][96] The latter is based on the successful measurement of the dust electric charge by CDA.[88][89] A dust Trajectory Sensor consists of four planes of parallel position sensing wire electrodes.[97] Dust accelerator tests show that dust trajectories can be determined to an accuracy of 1% in velocity and 1° in direction.[98] The second element of a Dust Telescope is a Large-area Mass Analyzer.[99] A Large-area Mass Analyzer is a reflectron type time-of-flight mass analyzer of up to 0.2 m2 sensitive area[100] of mass resolution R > 150. It consists of a circular plate target with the ion detector behind the center hole. In font of the target is an acceleration grid. Ions generated by an impact are reflected by a paraboloid shaped grid onto the center ion detector. Prototypes of dust telescope have been built at the Laboratory for Atmospheric and Space Physics (LASP) of the University of Colorado in Boulder (USA)[101] and at the Institute of Space Systems[102] of the University of Stuttgart and tested at their dust accelerators.[103]
The Surface Dust Analyser (SUDA) on board the Europa Clipper mission, is being developed by Sacha Kempf and colleagues at (LASP). SUDA will collect spatially resolved compositional maps of Europa along the ground tracks of the Europa orbiter and search for plumes. The instrument is capable of identifying traces of organic and inorganic compounds in the ice ejecta.[104] Launch of the Europa Clipper mission is planned for 2024.[105]
The DESTINY+ Dust Analyzer (DDA) will fly on the Japanese-German space mission Destiny+ to asteroid 3200 Phaethon.[106][107] Phaethon is believed to be the origin of the Geminids meteor stream that can be observed from the ground every December. DDA[108] development is led by Ralf Srama and colleagues from the Institute of Space Systems (IRS)[109] at the University of Stuttgart in cooperation with von Hoerner & Sulger GmbH (vH&S) company.[110] DDA's will analyze interstellar and interplanetary dust on cruise to Phaethon[111] and will study its dust environment during the encounter; of particular interest is the proportion of organic matter. Launch is planned for 2024.
The Interstellar Dust Experiment (IDEX)[112] will fly on the Interstellar Mapping and Acceleration Probe (IMAP) in orbit about the Sun–Earth L1 Lagrange point. IDEX is developed by Mihaly Horanyi and colleagues at the Laboratory for Atmospheric and Space Physics (LASP) at the University of Colorado Boulder. IDEX is a large-area (0.07 m2) dust analyzer that provides the mass distribution and elemental composition of interstellar and interplanetary dust particles. A laboratory version of the IDEX instrument was used at the dust accelerator facility[113] operated at University of Colorado to collect impact ionization mass spectra for a range of dust samples of known composition.[114] Launch is planned for 2025.
Collected dust analyses
The importance of lunar samples and lunar soil for dust science was that they provided a meteoroid impact cratering record. Even more important are cosmochemical aspects. From their isotopic, elemental, molecular, and mineralogical compositions important conclusions about e.g. the origin of the Moon like the giant-impact hypothesis[115] can be drawn. From 1969 to 1972 six Apollo missions collected 382 kilograms of lunar rocks and soil. These samples are available for research and teaching projects.[116] From 1970 to 1976 three Luna spacecraft returned 301 grams lunar material. Recently, in 2020 Chang'e 5 collected 1,7 kg of lunar material.
In 1950 Fred Whipple showed that micrometeoroid smaller than a critical size (~100 micrometers) are decelerated at altitudes > 100 km slowly enough to radiate the frictional power away without melting.[117] Such micrometeorites sediment through the atmosphere and, finally, deposit on the ground. The most efficient method to collect micrometeorites is by high (~20 km) flying aircraft with special silicon oil covered collectors that capture this dust. At lower altitudes these micrometeorites become mixed with Earth dust. Don Brownlee first reliably identified the extraterrestrial nature of collected dust particles by their chondritic composition.[118] These stratospheric dust samples are available for further research.[119]
Stardust was the first mission to return samples from a comet (Wild 2) and from interstellar space. In January 2004, Stardust flew by Comet Wild 2 at a distance of 237 km with a relative velocity of 6.1 km/s. One side of the 0.104 m2 aerogel and 0.015 m2 aluminium foil dust collector [120] was exposed to the flow of cometary dust. The Stardust cometary samples were a mix of different components that included presolar grains like 13C-rich SiC grains, a wide range of chondrule-like fragments, and high temperature condensates like calcium-aluminum inclusions (CAIs) found in primitive meteorites that were transported to cold nebular regions. [121] From March to May 2000 and from July to December 2002 the spacecraft was in favourable position to collect interstellar dust on the back side of the sample collector. After return of the sample return capsule in January 2006 the collector trays were inspected and thousands of grains from Comet Wild 2[122] and seven probable interstellar grains[123] were identified. These grains are available for teaching and research from the NASA Astromaterials Curation Office[124]
The first asteroid samples were returned by the JAXA Hayabusa missions. Hyabusa encountered asteroid 25143 Itokawa in November 2005, picked up surface samples, and returned to Earth in June 2010. Despite some problems during sample collection thousands 10 to 100 micron sized particles are available for research in the laboratories.[125] The second Hayabusa2 mission rendezvoused with asteroid 162173 Ryugu in June 2018. About 5 g surface and sub-surface material from this primitive C-type asteroid were returned.[126] About 10% of the collected samples JAXA is sharing with NASA sample curation.[127][128]
The Rosetta space probe orbited comet 67P/Churyumov–Gerasimenko from August 2014 to September 2016. During this time Rosetta's instruments analyzed the nucleus, the dust, gas, and plasma environment. Rosetta carried a suite of miniaturized sophisticated lab instruments to study collected cometary dust particles. Among them was the high-resolution secondary ion mass spectrometer COSIMA (Cometary Secondary Ion Mass Analyzer) that analyzed the rocky and organic composition of collected dust particles,[129][130] an atomic force microscope MIDAS (Micro-Imaging Dust Analysis System) that investigated morphology and physical properties of micrometer-sized dust particles that were deposited on a collector plate,[131] and the double-focus magnetic mass spectrometer (DFMS) and the reflectron type time of flight mass spectrometer (RTOF) of ROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis) to analyze cometary gas and the volatile components of cometary particulates.[132][133] Rosetta's Philae lander carried the gas chromatography–mass spectrometry COSAC experiment to analyze organic molecules in the comet's atmosphere and on its surface[134]
See also
- Cosmic Dust Analyzer
- Galileo and Ulysses Dust Detectors
- Helios Dust Instrumentation
- Surface Dust Analyser
- Venetia Burney Student Dust Counter
References
- ^ McCracken, C.W.; Alexander, W.M.; Dubin, M. (November 1961). "Direct Measurement of Interplanetary Dust Particles in the Vicinity of Earth". Nature. 192 (4801): 441–442. Bibcode:1961Natur.192..441M. doi:10.1038/192441b0. S2CID 4206906. Retrieved 2 March 2022.
- ^ McCracken, C.W.; Alexander, W.M. (1963). "The distribution of small interplanetary dust particles in the vicinity of Earth". Smithsonian Contributions to Astrophysics. 7: 71. Bibcode:1963SCoA....7...71M. Retrieved 2 March 2022.
- ^ Nazarova, T.N. (July 1968). "Solid Component of Interplanetary Matter from Vehicle Observations". Space Science Reviews. 8 (3): 455–466. Bibcode:1968SSRv....8..455N. doi:10.1007/BF00184742. S2CID 121139277. Retrieved 2 March 2022.
- ^ Elsässer, H. (September 1963). "The zodiacal light". Planetary and Space Science. 11 (9): 1015–1033. Bibcode:1963P&SS...11.1015E. doi:10.1016/0032-0633(63)90040-0. Retrieved 2 March 2022.
- ^ Nilsson, C. (September 1966). "Some Doubts about the Earth's Dust Cloud". Science. 193 (3741): 1242–1246. Bibcode:1966Sci...153.1242N. doi:10.1126/science.153.3741.1242. S2CID 21191301. Retrieved 2 March 2022.
- ^ Fechtig, H.; Leinert, Ch.; Berg, O. (2001). Historical Perspectives. Historical Perspectives. Astronomy and Astrophysics Library. Springer,com. pp. 1–55. doi:10.1007/978-3-642-56428-4_1. ISBN 978-3-642-62647-0. Retrieved 23 March 2022.
- ^ Grün, E.; Gustafson, B.A.S.; Dermott, S.; Fechtig, H. (2001). Interplanetary Dust. Berlin: Springer. Bibcode:2001indu.book.....G. ISBN 978-3-540-42067-5. Retrieved 5 February 2022.
- ^ Veysset, D.; Lee, J-H.; Hassani, M.; Kooi, S.; Thomas, E.; Nelson, K. (March 2021). "High-velocity micro-projectile impact testing". Applied Physics Reviews. 6 (1): article id.011319. Bibcode:2021ApPRv...8a1319V. doi:10.1063/5.0040772. hdl:1721.1/141164. S2CID 234356185. Retrieved 23 May 2022.
- ^ "Experimental Impact Laboratory" (PDF). JSC Experimental Impact Laboratory. Retrieved 27 April 2022.
- ^ Hibbert, R.; Cole, M.J.; Price, M.C.; Burchel, M.J. (2017). "The Hypervelocity Impact Facility at the University of Kent: Recent Upgrades and Specialized Capabilities" (PDF). Procedia Engineering. 204: 208. doi:10.1016/j.proeng.2017.09.775. Retrieved 27 April 2022.
- ^ Shelton, H.; Hendricks, C.D.; Wuerker, RF (1960). "Electrostatic Acceleration of Microparticles to Hypervelocities". Journal of Applied Physics. 31 (7): 1243. Bibcode:1960JAP....31.1243S. doi:10.1063/1.1735813. Retrieved 27 April 2022.
- ^ "IRS".
- ^ Mocker, A.; Bugiel, S.; Auer, S.; Baust, G.; Collette, A.; Drake, K.; Fiege, K.; Grün, E.; Heckmann, F.; Helfert, S.; Hillier, J.; Kempf, S.; Matt, G.; Mellert, T.; Munsat, T.; Otto, K.; Postberg, F.; Röser, H. P.; Shu, A.; Strernovski, Z.; Srama, R. (September 2011). "A 2 MV Van de Graaff accelerator as a tool for planetary and impact physics research". Review of Scientific Instruments. 82 (9): 95111-95111-8. Bibcode:2011RScI...82i5111M. doi:10.1063/1.3637461. PMID 21974623. Retrieved 27 April 2022.
- ^ Shu, A.; Colette, A.; Drake, K.; Grün, E.; Horanyi, M.; Kempf, S.; Mocker, A.; Munsat, T.; Northway, P.; Srama, R.; Sterbovski, Z.; Thomas, E. (July 2012). "3 MV hypervelocity dust accelerator at the Colorado Center for Lunar Dust and Atmospheric Studies". Review of Scientific Instruments. 83 (7): 075108-075108-8. Bibcode:2012RScI...83g5108S. doi:10.1063/1.4732820. PMID 22852725. Retrieved 27 April 2022.
- ^ "LASP dust accelerator facility". Retrieved 23 May 2022.
- ^ Neukum, G.; Mehl, A.; Fechtig, H.; Zähringer, J. (March 1970). "Impact phenomena of micrometeorites on lunar surface material". Earth and Planetary Science Letters. 9 (1): 31. Bibcode:1970E&PSL...8...31N. doi:10.1016/0012-821X(70)90095-6. Retrieved 27 April 2022.
- ^ Grün, E.; Fechtig, H.; Hanner, M.; Kissel, J.; Lindblad, B.A.; Linkert, D.; Maas, D.; Morfill, G.E.; Zook, H. (May 1992). "The Galileo Dust Detector". Space Science Reviews. 60 (1–4): 317–340. Bibcode:1992SSRv...60..317G. doi:10.1007/BF00216860. Retrieved 11 February 2022.
- ^ Thomas, E.; Simolka, J.; DeLuca, M.; Horanyi, M.; Janches, D.; Marshall, R; Munsat, T.; Plane, J.; Sternovski, Z. (March 2017). "Experimental setup for the laboratory investigation of micrometeoroid ablation using a dust accelerator". Review of Scientific Instruments. 88 (3): id.034501. Bibcode:2017RScI...88c4501T. doi:10.1063/1.4977832. PMID 28372412. Retrieved 27 April 2022.
- ^ Vedder, J.F. (January 1978). "Microparticle accelerator of unique design". Review of Scientific Instruments. 49 (1): 1. Bibcode:1978RScI...49....1V. doi:10.1063/1.1135244. PMID 18698928. Retrieved 23 May 2022.
- ^ Dalmann, B; Grün, E.; Kissel, J.; Dietzel, H. (August 1978). "The ion-composition of the plasma produced by impacts of fast dust particles". Planetary and Space Science. 25 (2): 135. Bibcode:1977P&SS...25..135D. doi:10.1016/0032-0633(77)90017-4. Retrieved 23 May 2022.
- ^ Naumann, R.J. (December 1, 1965). "Pegasus satellite measurements of meteoroid penetration /February 16 - July 20, 1965/". NTRS - NASA Technical Reports Server. NASA TM. Retrieved 4 March 2022.
- ^ Grün, E.; Berg, O.E.; Dohnanyi, J.S. (1973). "Reliability of cosmic dust data from Pioneers 8 and 9". Space Research XIII. 2: 1057–1062. Bibcode:1973spre.conf.1057G. Retrieved 5 March 2022.
- ^ Hoffmann, H.J.; Fechtig, H.; Grün, E.; Kissel, J. (January 1975). "First results of the micrometeoroid experiment s 215 on the HEOS 2 satellite". Planetary and Space Science. 23 (1): 215–224. Bibcode:1975P&SS...23..215H. doi:10.1016/0032-0633(75)90080-X. Retrieved 5 March 2022.
- ^ Morrison, D.A.; Zinner, E. (1977). "12054 and 76215: new measurements of interplanetary dust and solar flare fluxes". Lunar Science Conference, 8th, Houston, Tex., March 14–18, 1977, Proceedings. 1: 841. Bibcode:1977LPSC....8..841M. Retrieved 25 May 2022.
- ^ Morrison, D.A.; Clanton, U.S. (1979). "Properties of microcraters and cosmic dust of less than 1000 Å dimensions". In: Lunar and Planetary Science Conference, 10th, Houston, Tex., March 19–23, 1979, Proceedings. 2: 1649. Bibcode:1979LPSC...10.1649M. Retrieved 25 May 2022.
- ^ Hörz, F.; Morrison, D.A.; Brownlee, D.E.; Fechtig, H.; Hartung, J.B.; Neukum, G.; Schneider, E.; Vedder, J.F.; Gault, D.E. (January 1975). "Lunar microcraters: Implications for the micrometeoroid complex". Planetary and Space Science. 23 (1): 151. Bibcode:1975P&SS...23..151H. doi:10.1016/0032-0633(75)90076-8. Retrieved 25 May 2022.
- ^ a b Grün, E.; Zook, H.A.; Fechtig, H.; Giese, R.H. (May 1985). "Collisional balance of the meteoritic complex". Icarus. 62 (2): 244–272. Bibcode:1985Icar...62..244G. doi:10.1016/0019-1035(85)90121-6. Retrieved 23 January 2022.
- ^ Love, s:g; Brownlee, D.A. (October 1993). "A Direct Measurement of the Terrestrial Mass Accretion Rate of Cosmic Dust". Science. 262 (5133): 550–553. Bibcode:1993Sci...262..550L. doi:10.1126/science.262.5133.550. PMID 17733236. S2CID 35563939. Retrieved 25 May 2022.
- ^ McDonnell, J.A.M.; the Canterbury LDEF MAP team (1992). "Impact cratering from LDEF's 5.75-year exposure: decoding of the interplanetary and earth-orbital populations". Proceedings of Lunar and Planetary Science, Volume 22; Conference, Houston, TX, Mar. 18-22, 1991 (A92-30851 12-91). Houston, TX, Lunar and Planetary Institute. 22: 185. Bibcode:1992LPSC...22..185M. Retrieved 25 May 2022.
- ^ Leinert, C; Hanner, M.; Pitz, E (February 1978). "On the spatial distribution of interplanetary dust near 1 AU". Astronomy and Astrophysics. 63 (1–2): 183. Bibcode:1978A&A....63..183L. Retrieved 30 May 2022.
- ^ Hanner, M.S.; Sparrow, J.G.; Weinberg, J.L.; Beeson, D.E. (1976). "Pioneer 10 observations of zodiacal light brightness near the ecliptic: Changes with heliocentric distance". Conference Proceedings: Interplanetary Dust and Zodiacal Light. Lecture Notes in Physics. 48: 24. Bibcode:1976LNP....48...29H. doi:10.1007/3-540-07615-8_448. ISBN 978-3-540-07615-5. Retrieved 31 May 2022.
- ^ Soberman, R.K.; Neste, S.I.; Petty, A.F. (1971). "Asteriod Detection from Pioneers F and G". Physical Studies of Minor Planets, Proceedings of IAU Colloq. 12, Held in Tucson, AZ, March, 1971. 267: 617. Bibcode:1971NASSP.267..617S. Retrieved 1 June 2022.
- ^ a b Auer, S.; Soberman, R.K.; Neste, S.L.; Lichtenberg, K (1974). "The Asteroid Belt: Doubts about the Particle Concentration Measured with the Asteroid/Meteoroid Detector on Pioneer 10". Science. 186 (4164): 650–652. Bibcode:1974Sci...186..650A. doi:10.1126/science.186.4164.650. JSTOR 1739199. PMID 17833722. Retrieved 1 June 2022.
- ^ Kelsall, T.; Weiland, J.L.; Franz, B.A.; Reach, W.T.; Arendt, R.G.; Dwek, F.; Freudenreich, H.T.; Hauser, M.G.; Moseley, S,H; Odegard, N.P.; Silverberg, R.F.; Wright, E.L. (November 1998). "The COBE Diffuse Infrared Background Experiment Search for the Cosmic Infrared Background. II. Model of the Interplanetary Dust Cloud" (PDF). The Astrophysical Journal. 508 (1): 44–73. arXiv:astro-ph/9806250. Bibcode:1998ApJ...508...44K. doi:10.1086/306380. S2CID 17673274. Retrieved 31 May 2022.
- ^ "COBE Images". COBE Slide Set - High-Resolution Images. NASA Goddard Space Flight Center. Retrieved 1 June 2022.
- ^ Sykes, M.; Walker, R. (February 1992). "Cometary dust trails I. Survey". Icarus. 95 (2): 180. Bibcode:1992Icar...95..180S. doi:10.1016/0019-1035(92)90037-8. Retrieved 1 June 2022.
- ^ Reach, W.T.; Kelley, M.S.; Sykes, M. (November 2007). "A survey of debris trails from short-period comets". Icarus. 191 (1): 298. arXiv:0704.2253. Bibcode:2007Icar..191..298R. doi:10.1016/j.icarus.2007.03.031. S2CID 18970907. Retrieved 1 June 2022.
- ^ Soja, R.; Grün, E.; Srama, R.; Sterkem, V.; Vaubaillon, J.; Krüger, H.; Sommer, M.; Herzog, J.; Hornig, A.; Bausch, L. "IMEX – Interplanetary Meteoroid Environment for eXploration" (PDF). ESA. Retrieved 1 June 2022.
- ^ "Dust trail of comet 67P/Churyumov-Gerasimenko". Tracing the dust trails of Comet 67P/Churyumov-Gerasimenko. ESA. Retrieved 1 June 2022.
- ^ a b Naumann, R.J. (November 1966). "The Near-Earth Meteoroid Environment". Rep. NASA Tech. Note, NASA-TN-D-3717. 3717. Bibcode:1966NASTN3717.....N. Retrieved 6 June 2022.
- ^ Humes, D.H. (November 1980). "Results of Pioneer 10 and 11 Meteoroid Experiments: Interplanetary and Near-Saturn". Journal of Geophysical Research. 85 (A11): 5841. Bibcode:1980JGR....85.5841H. doi:10.1029/JA085iA11p05841. Retrieved 6 June 2022.
- ^ Naumann, R.J. "Pegasus satellite measurements of meteoroid penetration (Feb. 16 - July 20, 1965)" (PDF). NTRS - NASA Technical Reports Server. NASA. Retrieved 7 June 2022.
- ^ Simpson, J.A; Sagdeev, R.Z.; Tuzzolino, A.J.; Perkins, M.A.; Ksanfomality, L.V.; Rabinowitz, D.; Lentz, G.A.; Afonin, V.V.; Ero, J.; Keppler, E.; Kosorokov, J.; Petrova, F.; Scabo, L.; Umlauft, G. (May 1986). "Dust counter and mass analyser (DUCMA) measurements of comet Halley's coma from Vega spacecraft". Nature. 321: 278. Bibcode:1986Natur.321..278S. doi:10.1038/321278a0. S2CID 122995125. Retrieved 7 June 2022.
- ^ James, D.; Hoxie, V.; Horanyi, M. (March 2010). "Polyvinylidene fluoride dust detector response to particle impacts". Review of Scientific Instruments. 81 (3): 34501. Bibcode:2010RScI...81c4501J. doi:10.1063/1.3340880. PMID 20370201. Retrieved 7 June 2022.
- ^ Kempf, S.; Beckmann, U.; Moragas-Klostermeyer, G.; Postberg, F.; Srama, R.; Economou, T.; Schmidt, J.; Spahn, F.; Grün, E. (February 2008). "The E ring in the vicinity of Enceladus. I. Spatial distribution and properties of the ring particles". Icarus. 193 (2): 420. Bibcode:2008Icar..193..420K. doi:10.1016/j.icarus.2007.06.027. Retrieved 7 June 2022.
- ^ Piquett, M.; Poppe, A.R.; Bernadoni, E.; Szalay, J.R.; James, D.; Horanyi, M.; Stern, S.A.; Weaver, H.; Spencer, J.; Olkin, C.; New Horizons P&P Team (March 2019). "Student Dust Counter: Status report at 38 AU". Icarus. 321: 116. Bibcode:2019Icar..321..116P. doi:10.1016/j.icarus.2018.11.012. S2CID 125115666. Retrieved 7 June 2022.
- ^ McDonnell, J.A.M. (June 1987). "The Giotto dust impact detection system". Journal of Physics E: Scientific Instruments. 20 (6): 741. Bibcode:1987JPhE...20..741M. doi:10.1088/0022-3735/20/6/033. Retrieved 7 June 2022.
- ^ McDonnell, J.A.M.; Evans, G.C.; Evans, S.T.; Alexander, W,M; Burton, W,M; Fith, J.G.; Bussoletti, E.; Grard, R.J.; Hanner, M.S.; Sekanina, Z.; Stevenson, T.J.; Turner, R.F.; Weishaupt, U.; Wallis, M.K.; Zarnecki, J.C. (November 1987). "The dust distribution within the inner coma of comet P/Halley 1982i - Encounter by Giotto's impact detectors". Astronomy and Astrophysics. 17 (1): 719. Bibcode:1987A&A...187..719M. Retrieved 7 June 2022.
- ^ McDonnell, J.A.M.; McBride, N.; Beard, R.; Bussoletti, E.; Colangeli, L.; Eberhardt, P.; Firth, J.G.; Grard, R.; Green, S.F.; Greenberg, J.M. (April 1993). "Dust particle impacts during the Giotto encounter with comet Grigg-Skjellerup". Nature. 362 (6422): 732. Bibcode:1993Natur.362..732M. doi:10.1038/362732a0. S2CID 4363877. Retrieved 7 June 2022.
- ^ "Mercury Magnetospheric Orbiter". ESA Science Missions. ESA. Retrieved 15 June 2022.
- ^ "Mercury Dust Monitor". ESA Science Missions. ESA. Retrieved 15 June 2022.
- ^ Kobayashi, M.; Shibata, H.; Nogami, K; Fujii, M; Hasegawa, S.; Hirabayashi, M.; Hirai, T.; Iwai, T.; Kimura, H.; Kimura, T.; Nakamura, M.; Ohashi, H.; Sasaki, S.; Takechi, S.; Yano, H.; Krüger, H.; Lohse, A.K.; Srama, R.; Strub, P.; Grün, E. (December 2020). "Mercury Dust Monitor (MDM) Onboard the Mio Orbiter of the BepiColombo Mission". Space Science Reviews. 216 (8): 144. Bibcode:2020SSRv..216..144K. doi:10.1007/s11214-020-00775-7. S2CID 230629869. Retrieved 7 June 2022.
- ^ Gurnett, D.A.; Grün, E.; Gallagher, D.; Kurth, W.S.; Scarf, F.L. (February 1983). "Micron-sized particles detected near Saturn by the Voyager plasma wave instrument". Icarus. 53 (2): 236. Bibcode:1983Icar...53..236G. doi:10.1016/0019-1035(83)90145-8. Retrieved 17 June 2022.
- ^ Srama, R.; Kempf, S.; Moragas.Klostermeyer, G.; Helfert, S.; Ahrens, T.J.; Altobelli, N.; Auer, S.; Beckmann, U.; Bradley, J.G.; Burton, M.; Dikarev, V.; Economou, T; Fechtig, H.; Green, S.F.; Gande, M.; Havnes, O; Hillier, J.K.; Horanyi, M.; Igenbergs, E.; Jessberger, E.K.; Johnson, T.V.; Krüger, H.; Matt, G.; McBride, N.; Mocker, A.; Lamy, P.; Linkert, D.; Linkert, G.; Lura, F.; McDonnell, J.A.M.; Möhlmann, D.; Morfill, G.E.; Postberg, F.; Roy, M.; Schwehm, G.; Spahn, F; Svestka, J.; Tschernjawski, V.; Tuzzolino, A.J.; Wäsch, R.; Grün, E. (August 2006). "In situ dust measurements in the inner Saturnian system". Planetary and Space Science. 54 (9): 967. Bibcode:2006P&SS...54..967S. doi:10.1016/j.pss.2006.05.021. Retrieved 18 June 2022.
- ^ Gurnett, D.A.; Kurth, W.S.; Scarf, F.K.; Burns, J.A.; Cuzzi, J.N.; Grün, E. (December 1987). "Micron-sized particle impacts detected near Uranus by the Voyager 2 plasma wave instrument". Journal of Geophysical Research. 92 (A13): 14959. Bibcode:1987JGR....9214959G. doi:10.1029/JA092iA13p14959. Retrieved 17 June 2022.
- ^ Gurnett, D.A.; Kurth, S.W.; Granroth, L.J.; Allendorf, S.C.; Poynter, R.L. (October 1991). "Micron-size particles detected near Neptune by the Voyager 2 plasma wave instrument". Journal of Geophysical Research. 96: 19177. Bibcode:1991JGR....9619177G. doi:10.1029/91JA01270. Retrieved 17 June 2022.
- ^ Gurnett, D.A.; Averkamp, T.F.; Scarf, F.L.; Grün, E. (March 1986). "Dust particles detected near Giacobini-Zinner by the ICE Plasma Wave Instrument". Geophysical Research Letters. 13 (3): 291. Bibcode:1986GeoRL..13..291G. doi:10.1029/GL013i003p00291. Retrieved 17 June 2022.
- ^ Shen, M.M.; Sternovsky, Z.; Garzelli, Â.; Malaspina, D.M. (September 2021). "Electrostatic Model for Antenna Signal Generation From Dust Impacts". Journal of Geophysical Research: Space Physics. 126 (9): article id. e29645. Bibcode:2021JGRA..12629645S. doi:10.1029/2021JA029645. S2CID 237692026. Retrieved 17 June 2022.
- ^ Berg, O.E.; Rischardson, F.F. (1969). "The Pioneer 8 cosmic dust experiment". Review of Scientific Instruments. 40 (10): 1333–1337. Bibcode:1969RScI...40.1333B. doi:10.1063/1.1683778. hdl:2060/19690021680. Retrieved 3 July 2022.
- ^ Zook, H.; Berg, O.E. (January 1975). "A source for hyperbolic cosmic dust particles". Planetary and Space Science. 23 (4): 183–203. Bibcode:1975P&SS...23..183Z. doi:10.1016/0032-0633(75)90078-1. Retrieved 3 July 2022.
- ^ Dietzel, G; Fechtig, H.; Grün, E.; Hoffmann, H.J.; Kissel, J. (March 1973). "The HEOS 2 and HELIOS micrometeoroid experiments". Journal of Physics E: Scientific Instruments. 6 (3): 209–217. Bibcode:1973JPhE....6..209D. doi:10.1088/0022-3735/6/3/008. Retrieved 18 June 2022.
- ^ Fechtig, H.; Grün, E.; Morfill, G.E. (April 1979). "Micrometeoroids within ten Earth radii". Planetary and Space Science. 27 (4): 511–531. Bibcode:1979P&SS...27..511F. doi:10.1016/0032-0633(79)90128-4. Retrieved 11 February 2022.
- ^ Grün, E.; Staubach, P.; Baguhl, M.; Hamilton, D.P.; Zook, H.; Dermott, S.; Gustafson, B.A.; Fechtig, H.; Kissel, J.; Linkert, D.; Linkert, G.; Srama, R.; Hanner, M.S.; Polanskey, C.; Horanyi, M.; Lindblad, B.A.; Mann, I.; McDonnell, J.A.M.; Morfill, G.; Schwehm, G. (October 1997). "South-North and Radial Traverses through the Interplanetary Dust Cloud". Icarus. 129 (2): 270–288. Bibcode:1997Icar..129..270G. doi:10.1006/icar.1997.5789. Retrieved 12 February 2022.
- ^ a b Grün, E.; Zook, H.A.; Baguhl, M.; Balogh, A.; Bame, S.J.; Fechtig, H.; Forsyth, R.; Hanner, M.S.; Horanyi, M.; Kissel, J.; Lindblad, B.A.; Linkert, D.; Linkert, G.; Mann, I.; McDonnell, J.A.M.; Morfill, G.E.; Phillips, J.L.; Polanskey, C.; Schwehm, G.; Siddique, N. (April 1993). "Discovery of Jovian dust streams and interstellar grains by the Ulysses spacecraft". Nature. 362 (6419): 428–430. Bibcode:1993Natur.362..428G. doi:10.1038/362428a0. S2CID 4315361. Retrieved 23 January 2022.
- ^ Krüger, H.; Krivov, A.V.; Sremsevic, M.; Grün, E. (July 2003). "Impact-generated dust clouds surrounding the Galilean moons". Icarus. 164 (1): 170–187. arXiv:astro-ph/0304381. Bibcode:2003Icar..164..170K. doi:10.1016/S0019-1035(03)00127-1. S2CID 6788637. Retrieved 29 January 2022.
- ^ Horanyi, M.; Sternovsky, Z.; Lankton, M.; Dumont, C.; Gagnard, S.; Gathright, D.; Grün, E.; Hansen, D.; James, D.; Kempf, S.; Lamprecht, B.; Srama, R.; Szalay, J.; Wright, G. (December 2014). "The Lunar Dust Experiment (LDEX) Onboard the Lunar Atmosphere and Dust Environment Explorer (LADEE) Mission". Space Science Reviews. 185 (1–4): 93. Bibcode:2014SSRv..185...93H. doi:10.1007/s11214-014-0118-7. S2CID 18649518. Retrieved 6 July 2022.
- ^ Horanyi, M.; Szalay, J.; Kempf, S.; Schmidt, J.; Grün, E.; Srama, R.; Sternovsky, Z. (June 2015). "A permanent, asymmetric dust cloud around the Moon". Nature. 522 (7556): 324–326. Bibcode:2015Natur.522..324H. doi:10.1038/nature14479. PMID 26085272. S2CID 4453018. Retrieved 6 July 2022.
- ^ Szalay, J.; Horanyi, M. (May 2016). "Lunar meteoritic gardening rate derived from in situ LADEE/LDEX measurements". Geophysical Research Letters. 43 (10): 4893–4898. Bibcode:2016GeoRL..43.4893S. doi:10.1002/2016GL069148. S2CID 132133302. Retrieved 7 July 2022.
- ^ Szalay, J.; Pokorny, P.; Jenniskens, P.; Horanyi, M. (March 2018). "Activity of the 2013 Geminid meteoroid stream at the Moon". Monthly Notices of the Royal Astronomical Society. 474 (3): 4225–4231. Bibcode:2018MNRAS.474.4225S. doi:10.1093/mnras/stx3007. PMC 5846084. PMID 29545651. Retrieved 7 July 2022.
- ^ Grün, E.; Fechtig, H.; Gammelin, P.; Kissel, J (October 1975). "Das Staubexperiment auf Helios (E10)". Raumfahrtforschung. 19: 268. Bibcode:1975RF.....19..268G. Retrieved 2 May 2022.
- ^ Dalmann, B.K.; Grün, E.; Kissel, J.; Dietzel, H. (February 1977). "The ion-composition of the plasma produced by impacts of fast dust particles". Planetary and Space Science. 25 (2): 135–147. Bibcode:1977P&SS...25..135D. doi:10.1016/0032-0633(77)90017-4. Retrieved 18 June 2022.
- ^ Pailer, N.; Grün, E. (March 1980). "The penetration limit of thin films". Planetary and Space Science. 28 (3): 321–331. Bibcode:1980P&SS...28..321P. doi:10.1016/0032-0633(80)90021-5. Retrieved 18 June 2022.
- ^ Grün, E.; Pailer, N; Fechtig, H.; Kissel, J. (March 1980). "Orbital and physical characteristics of micrometeoroids in the inner solar system as observed by Helios 1". Planetary and Space Science. 28 (3): 333–349. Bibcode:1980P&SS...28..333G. doi:10.1016/0032-0633(80)90022-7. Retrieved 29 June 2022.
- ^ Krüger, H.; Strub, P.; Sommer, M.; Altobelli, N.; Kimura, H.; Lohse, A.K.; Grün, E.; Srama, R. (November 2020). "Helios spacecraft data revisited: detection of cometary meteoroid trails by following in situ dust impacts" (PDF). Astronomy & Astrophysics. 643 (id. A96): 13. Bibcode:2020A&A...643A..96K. doi:10.1051/0004-6361/202038935. S2CID 225014796. Retrieved 2 July 2022.
- ^ Altobelli, N.; Grün, E.; Landgraf, M. (March 2006). "A new look into the Helios dust experiment data: presence of interstellar dust inside the Earth's orbit" (PDF). Astronomy and Astrophysics. 448 (1): 243. Bibcode:2006A&A...448..243A. doi:10.1051/0004-6361:20053909. S2CID 124533915. Retrieved 2 July 2022.
- ^ Kissel, J. (1986). "The Giotto Particulate Impact Analyser". ESA Spec. Publ., ESA SP-1077. 1070: 67–83. Bibcode:1986ESASP1070...67K.
- ^ Kissel, J.; Brownlee, D.; Clark, B.; Fechtig, H.; Grün, E.; Hornung, K.; Igenbergs, E; Jessberer, E.; Krüger, F.; Kuczera, H.; McDonnelll, J.A.M.; Morfill, G.; Rahe, J.; Schwehm, G.; Sekanina, Z.; Utterbeck, N.; Völk, H.; Zook, H. (May 1986). "Composition of comet Halley dust particles from Giotto observations". Nature. 321: 336–337 (1986). Bibcode:1986Natur.321..336K. doi:10.1038/321336a0. S2CID 186245081. Retrieved 20 July 2022.
- ^ Kissel, J.; Sagdeev, R.Z.; et al. (May 1986). "Composition of comet Halley dust particles from Vega observations" (PDF). Nature. 321: 280–282 (1986). Bibcode:1986Natur.321..280K. doi:10.1038/321280a0. S2CID 122405233. Retrieved 20 July 2022.
- ^ Jessberger, E.; Christoforidis, A; Kissel, J. (April 1988). "Aspects of the major element composition of Halley's dust" (PDF). Nature. 323 (6166): 691–695 (1988). Bibcode:1988Natur.332..691J. doi:10.1038/332691a0. S2CID 4349968. Retrieved 20 July 2022.
- ^ Kissel, J.; Krueger, F. (April 1987). "The organic component in dust from comet Halley as measured by the PUMA mass spectrometer on board Vega 1" (PDF). Nature. 326 (6115): 755–760 (1987). Bibcode:1987Natur.326..755K. doi:10.1038/326755a0. S2CID 4358568. Retrieved 20 July 2022.
- ^ Kissel, J; Glasmachers, A.; Grün, E.; Henkel, H.; Höfner, H.; Haerendel, G.; von Hoerner, H.; Hornung, K.; Jessberger, E. K.; Krueger, F. R.; Möhlmann, D.; Greenberg, J. M.; Langevin, Y.; Silén, J.; Brownlee, D.; Clark, B. C.; Hanner, M. S.; Hoerz, F.; Sandford, S.; Sekanina, Z.; Tsou, P.; Utterback, N. G.; Zolensky, M. E.; Heiss, C. (2003). "Cometary and Interstellar Dust Analyzer for comet Wild 2". Journal of Geophysical Research. 108 (E10): 8114. Bibcode:2003JGRE..108.8114K. doi:10.1029/2003JE002091.
- ^ Kissel, J.; Makinen, T.; Schmidt, W.; Silen, J. (October 2011). "Mass-spectrometric Measurements of Dust at Comets Wild-2 and Tempel-1" (PDF). EPSC-DPS Joint Meeting 2011, Held 2–7 October 2011 in Nantes, France. 2011: 1338. Bibcode:2011epsc.conf.1338K. Retrieved 29 July 2022.
- ^ Kissel, J.; Krueger, F.; Silen, J.; Clark, B.C. (June 2004). "The Cometary and Interstellar Dust Analyzer at Comet 81P/Wild 2". Science. 304 (5678): 1774–1776. Bibcode:2004Sci...304.1774K. doi:10.1126/science.1098836. PMID 15205526. S2CID 37996161. Retrieved 29 July 2022.
- ^ Srama, R.; Ahrens, T.J.; Altobelli, N.; Auer, S.; Bradley, J.; Burton, M.; Dikarev, V.; Economou, T.; Fechtig, H.; Görlich, M.; Grande, M.; Grün, E.; Havnes, O.; Helfert, S.; Horanyi, M.; Igenbergs, E.; Jessberger, E.; Johnson, T.V.; Kempf, S.; Krivov, A.; Krüger, H.; Mocker-Ahlreep, A.; Moragas-Klostermeyer, G.; Lamy, P.; Landgraf, M.; Linkert, D.; Linkert, G.; Lura, F.; McDonnell, J.A.M.; Möhlmann, D.; Morfill, G.; Roy, M.; Schäfer, G.; Schlotzhauer, G.; Schwehm, G.; Spahn, F.; Stübig, M.; Svestka, J.; Tschernjawski, V.; Tuzzolino, A.; Wäsch, R.; Zook, H. (September 2004). "The Cassini Cosmic Dust Analyzer". Space Science Reviews. 114 (1–4): 465–518. Bibcode:2004SSRv..114..465S. doi:10.1007/s11214-004-1435-z. S2CID 53122588. Retrieved 19 February 2022.
- ^ Hillier, J.; Green, E.; McBride, N.; Altobelli, N.; Postberg, F.; Kempf, S.; Schwanenthal, J.; Srama, R.; McDonnell, J.A.M.; Grün, E. (October 2007). "Interplanetary dust detected by the Cassini CDA Chemical Analyser". Icarus. 190 (2): 643–654. Bibcode:2007Icar..190..643H. doi:10.1016/j.icarus.2007.03.024. Retrieved 22 February 2022.
- ^ Altobelli, N.; Kempf, S.; Landgraf, M.; Srama, R.; Dikarev, V.; Krüger, H.; Moragas-Klostermeyer, G.; Grün, E. (October 2003). "Cassini between Venus and Earth: Detection of interstellar dust". Journal of Geophysical Research. 108 (A10): 8032. Bibcode:2003JGRA..108.8032A. doi:10.1029/2003JA009874. Retrieved 22 February 2022.
- ^ Postberg, F.; Kempf, S.; Srama, R.; Green, S.; Hillier, J-; McBride, N.; Grün, E. (July 2006). "Composition of jovian dust stream particles". Icarus. 183 (1): 122–134. Bibcode:2006Icar..183..122P. doi:10.1016/j.icarus.2006.02.001. Retrieved 22 February 2022.
- ^ a b Kempf, S.; Srama, R.; Altobelli, N.; Auer, S.; Tschernjawski, V.; Bradley, J.; Burton, M.; Helfert, S.; Johnson, T.V.; Krüger, H.; Moragas-Klostermeyer, G.; Grün, E. (October 2004). "Cassini between Earth and asteroid belt: first in-situ charge measurements of interplanetary grains". Icarus. 171 (2): 317–335. Bibcode:2004Icar..171..317K. doi:10.1016/j.icarus.2004.05.017. Retrieved 22 February 2022.
- ^ a b Kempf, S.; Beckmann, U.; Srama, R.; Horanyi, M.; Auer, S.; Grün, E. (August 2006). "The electrostatic potential of E ring particles". Planetary and Space Science. 54 (9–10): 999–1006. Bibcode:2006P&SS...54..999K. doi:10.1016/j.pss.2006.05.012. Retrieved 25 February 2022.
- ^ Srama, R.; Kempf, S.; Moragas-Klostermeyer, G.; Helfert, S.; Ahrens, T.J.; Altobelli, N.; Auer, S.; Beckmann, U.; Bradley, J.; Burton, M.; Dikarev, V.; Economou, T.; Fechtig, H.; Green, S.; Grande, M.; Havnes, O.; Hillier, J.; Horanyi, M.; Igenbergs, E.; Jessberger, E.; Johnson, T.V.; Krüger, H.; Matt, G.; McBride, N.; Mocker, A.; Lamy, P.; Linkert, D.; Linkert, G.; Lura, F.; McDonnell, J.A.M.; Möhlmann, D.; Morfill, G.; Postberg, F.; Roy, M.; Schwehm, G.; Spahn, F.; Svestka, J.; Tschernjawski, V.; Tuzzolino, A.; Wäsch, R.; Grün, E. (August 2006). "In situ dust measurements in the inner Saturnian system". Planetary and Space Science. 54 (9–10): 967–987. Bibcode:2006P&SS...54..967S. doi:10.1016/j.pss.2006.05.021. Retrieved 25 February 2022.
- ^ Hillier, J.; Green, S.F.; McBride, N.; Schwanenthal, J.; Postberg, F.; Srama, R.; Kempf, S.; Moragas-Klostermeyer, G.; McDonnell, J.A.M.; Grün, E. (June 2007). "The composition of Saturn's E ring". Monthly Notices of the Royal Astronomical Society. 377 (4): 1588–1596. Bibcode:2007MNRAS.377.1588H. doi:10.1111/j.1365-2966.2007.11710.x. S2CID 124773731. Retrieved 25 February 2022.
- ^ Spahn, F.; Schmidt, J.; Albers, N.; Hörning, M.; Makuch, M.; Seiß, M.; Kempf, S.; Srama, R.; Dikarev, V.; Helfert, S.; Moragasd-Klostermeyer, G.; Krivov, A.; Sremcevic, M.; Tuzzolono, A.; Economou, T.; Grün, E. (March 2006). "Cassini Dust Measurements at Enceladus and Implications for the Origin of the E Ring". Science. 311 (5766): 1416–1418. Bibcode:2006Sci...311.1416S. doi:10.1126/science.1121375. PMID 16527969. S2CID 33554377. Retrieved 25 February 2022.
- ^ Postberg, F.; Schmidt, J.; Hillier, J.; Kempf, S.; Srama, R. (June 2011). "A salt-water reservoir as the source of a compositionally stratified plume on Enceladus". Nature. 474 (7353): 620–622. Bibcode:2011Natur.474..620P. doi:10.1038/nature10175. PMID 21697830. S2CID 4400807. Retrieved 25 February 2022.
- ^ Altobelli, N.; Postberg, F.; Fiege, K.; Trieloff, M.; Kimura, H.; Sterken, V.; Hsu, W.H.; Hillier, J.; Khawaja, N.; Moragas-Klostermeyer, G.; Blum, J.; Burton, M.; Srama, R.; Kempf, S.; Grün, E. (April 2016). "Flux and composition of interstellar dust at Saturn from Cassini's Cosmic Dust Analyzer". Science. 352 (6283): 312–318. Bibcode:2016Sci...352..312A. doi:10.1126/science.aac6397. PMID 27081064. S2CID 24111692. Retrieved 26 February 2022.
- ^ Grün, E.; Krüger, H.; Srama, R.; Auer, S.; Colangeli, L.; Horanyi, M.; Whitnell, P.; Kissel, J.; Landgraf, M.; Svedhem, H. (October 2000). "Dust Telescope: A New Tool for Dust Research". American Astronomical Society, DPS Meeting #32, Id.26.16; Bulletin of the American Astronomical Society. 32: 1043. Bibcode:2000DPS....32.2616G. Retrieved 1 August 2022.
- ^ Srama, R.; Srowig, A.; Rachev, M.; Grün, E.; Auer, S.; Conlon, T.; Glasmachers, A.; Harris, D.; Kempf, S.; Linnemeann, H.; Moragas-Klostermeyer, G.; Tschernjawski, V. (December 2004). "Development of AN Advanced Dust Telescope". Earth, Moon, and Planets. 95 (1–4): 211–220. Bibcode:2004EM&P...95..211S. doi:10.1007/s11038-005-9040-z. S2CID 121243309. Retrieved 1 August 2022.
- ^ Auer, S.; Grün, E.; Kempf, S.; Srama, R.; Srowig, A.; Sternovsky, Z.; Tschernjawski, V. (August 2008). "Characteristics of a dust trajectory sensor". Review of Scientific Instruments. 79 (8): 084501-084501-7 (2008). Bibcode:2008RScI...79h4501A. doi:10.1063/1.2960566. PMID 19044367. Retrieved 2 August 2022.
- ^ Xie, J.; Sternovsky, Z.; Grün, E.; Auer, S.; Duncan, N.; Drake, K.; Le, H.; Horanyi, M.; Srama, R. (October 2011). "Dust trajectory sensor: Accuracy and data analysis". Review of Scientific Instruments. 82 (10): 105104-105104-11 (2011). Bibcode:2011RScI...82j5104X. doi:10.1063/1.3646528. PMID 22047326. Retrieved 2 August 2022.
- ^ Rachev, M.; Srama, R.; Srowig, A.; Grün, E. (December 2004). "Large area mass analyzer". Nuclear Instruments and Methods in Physics Research Section A. 535 (1–2): 162–164. Bibcode:2004NIMPA.535..162R. doi:10.1016/j.nima.2004.07.121. Retrieved 2 August 2022.
- ^ Srama, R.; Kempf, S.; Moragas-Klostermeyer, G.; Landgraf, M.; Helfert, S.; Sternovsky, Z.; Rachev, M.; Grün, E. (January 2007). "Laboratory Tests of the Large Area Mass Analyser". Workshop on Dust in Planetary Systems (ESA SP-643). September 26–30, 2005, Kauai, Hawaii. 643: 209–212. Bibcode:2007ESASP.643..209S. Retrieved 2 August 2022.
- ^ Sternovsky, Z.; Grün, E.; Drake, K.; Xie, J.; Horanyi, M.; Srama, R.; Kempf, S.; Postberg, F.; Mocker, A.; Auer, S.; Krüger, H. (2011). "Novel Instrument for Dust Astronomy: Dust Telescope". Aerospace Conference, 2011: 1–8. doi:10.1109/AERO.2011.5747300. ISBN 978-1-4244-7350-2. S2CID 27532569. Retrieved 2 August 2022.
- ^ "Institute of Space Systems". Institute of Space Systems. University of Stuttgart. Retrieved 2 August 2022.
- ^ Srama, R.; Sternovsky, Z.; Kempf, S.; Horanyi, M.; Postberg, F.; Krüger, H.; Kobayashi, M.; Sterken, V. (September 2021). "Dust Telescopes for Dust Astronomy". 15th Europlanet Science Congress 2021, Held Virtually, 13–24 September 2021. Bibcode:2021EPSC...15..659S. doi:10.5194/epsc2021-659. S2CID 242295026. Retrieved 2 August 2022.
- ^ SUDA: A Dust Mass Spectrometer for Compositional Surface Mapping for a Mission to Europa (PDF). S. Kempf, N. Altobelli, C. Briois, E. Grün, M. Horanyi, F. Postberg, J. Schmidt, R. Srama, Z. Sternovsky, G. Tobie, and M. Zolotov. EPSC Abstracts Vol. 9, EPSC2014-229, 2014. European Planetary Science Congress 2014.
- ^ "Europa Clipper Mission". Europa Clipper. NASA. Retrieved 3 August 2022.
- ^ "DESTINY+". DESTINY+. JAXA.
- ^ "Germany and Japan begin new asteroid mission". DESTINY+. DLR.
- ^ "DDA". DESTINY+ Dust Analyze. Hoerner & Sulger GmbH.
- ^ "Die neue Asteroidenmission DESTINY+". News. University Stuttgart.
- ^ "von Hoerner & Sulger GmbH". vH-S. von Hoerner & Sulger GmbH.
- ^ Krüger, H.; Strub, P.; Srama, R.; Kobayashi, M.; Arai, T.; Kimura, H.; Hirai, T.; Moragas-Klostermeyer, G.; Altobelli, N.; Sterken, V.; Agarwal, J.; Sommer, M.; Grün, E. (August 2019). "Modelling DESTINY+ interplanetary and interstellar dust measurements en route to the active asteroid (3200) Phaethon" (PDF). Planetary and Space Science. 172: 22–42. arXiv:1904.07384. Bibcode:2019P&SS..172...22K. doi:10.1016/j.pss.2019.04.005. S2CID 118708512. Retrieved 3 August 2022.
- ^ "IDEX". Interstellar Dust Explorer. LASP.
- ^ "IMPACT". Institute for Modeling Plasma, Atmospheres and Cosmic Dust. LASP.
- ^ Sternovsky, Z.; Mikula, R.; Horanyi, M.; Hillier, J.; Srama, R.; Postberg, F. (December 2021). "Laboratory calibration of the Interstellar Dust Experiment (IDEX) instrument". AGU Fall Meeting 2021, Held in New Orleans, LA, 13-17 December 2021. id. SH25C-2108. Bibcode:2021AGUFMSH25C2108S.
- ^ Canup, R.; Asphaug, E. (August 2001). "Origin of the Moon in a giant impact near the end of the Earth's formation". Nature. 412 (6848): 708–712. Bibcode:2001Natur.412..708C. doi:10.1038/35089010. PMID 11507633. S2CID 4413525.
- ^ "Lunar Rocks and Soils from Apollo Missions". Curation/Lunar. NASA. Retrieved 8 July 2022.
- ^ Whipple, F. (December 1950). "The Theory of Micro-Meteorites. Part I. In an Isothermal Atmosphere". Proceedings of the National Academy of Sciences of the United States of America. 36 (12): 687–695. Bibcode:1950PNAS...36..687W. doi:10.1073/pnas.36.12.687. PMC 1063272. PMID 16578350.
- ^ Brownlee, D.E.; Tomandl, D.A.; Olszewski, E. (1977). "Interplanetary dust: a new source of extraterrestrial material for laboratory studies". Lunar Science Conference, 8th, Houston, Tex., March 14–18, 1977, Proceedings Volume 1. (A78-41551 18-91) New York, Pergamon Press, Inc. 1: 149–160. Bibcode:1977LPSC....8..149B. Retrieved 11 July 2022.
- ^ "Curation/Cosmic Dust". Stratospheric Dust Samples. NASA. Retrieved 10 July 2022.
- ^ Tsou, P.; Brownlee, D. E.; Sandford, S. A.; Horz, F.; Zolensky, M. E. (2003). "Wild 2 and interstellar sample collection and Earth return". Journal of Geophysical Research. 108 (E10): 8113. Bibcode:2003JGRE..108.8113T. doi:10.1029/2003JE002109.
- ^ Brownlee, D. (May 2014). "The Stardust Mission: Analyzing Samples from the Edge of the Solar System". Annual Review of Earth and Planetary Sciences. 42 (1): 179-205. Bibcode:2014AREPS..42..179B. doi:10.1146/annurev-earth-050212-124203. Retrieved 11 October 2022.
- ^ Brownlee, D.; Joswiak, D.; Mtrajt, G. (April 2012). "Overview of the rocky component of Wild 2 comet samples: Insight into the early solar system, relationship with meteoritic materials and the differences between comets and asteroids". Meteoritics & Planetary Science. 47 (4): 453–470. Bibcode:2012M&PS...47..453B. doi:10.1111/j.1945-5100.2012.01339.x. S2CID 128567869. Retrieved 11 July 2022.
- ^ Westphal, A.; et al. (September 2014). "Final reports of the Stardust Interstellar Preliminary Examination". Meteoritics & Planetary Science. 49 (9): 1720–1733. Bibcode:2014M&PS...49.1720W. doi:10.1111/maps.12221. S2CID 51735815. Retrieved 11 July 2022.
- ^ "Astromaterials Acquisition and Curation Office". Astromaterials Acquisition and Curation Office. NASA. Retrieved 11 July 2022.
- ^ Yoshikawa, M.; Kawaguchi, <j.; Fujiwara, A.; Tsuchiyama, A. (2015). "Hayabusa Sample Return Mission". Asteroids IV. Asteroids IV, Patrick Michel, Francesca e. DeMeo, and William F. Bottke (Eds.), University of Arizona Press, Tucson. pp. 397–418. Bibcode:2015aste.book..397Y. doi:10.2458/azu_uapress_9780816532131-ch021. ISBN 9780816532131. Retrieved 12 July 2022.
- ^ Yada, T.; et al. (December 2021). "Preliminary analysis of the Hayabusa2 samples returned from C-type asteroid Ryugu". Nature Astronomy. 6 (2): 214–220. Bibcode:2022NatAs...6..214Y. doi:10.1038/s41550-021-01550-6. S2CID 245366019. Retrieved 12 July 2022.
- ^ "Hayabusa Asteroid Itokawa Samples". Curation/Hayabusa. NASA. Retrieved 12 July 2022.
- ^ "Hayabusa2 Asteroid Ryugu Samples". Curation/Hayabusa2. NASA. Retrieved 12 July 2022.
- ^ Gardner, E; Lehto, H.; Lehto, K.; Fray, N.; Bardyn, A.; Lönnberg, T.; Merouane, S.; Isnard, R.; Cottin, H.; Hilchenbach, M.; and The Cosima Team (December 2020). "The detection of solid phosphorus and fluorine in the dust from the coma of comet 67P/Churyumov-Gerasimenko". Monthly Notices of the Royal Astronomical Society. 499 (2): 1870–1873. doi:10.1093/mnras/staa2950. Retrieved 15 July 2022.
- ^ Paquette, J.; Fray, N.; Bardyn, A.; Engrand, C.; Alexander, C.; Siljeström, S.; Cottin, H.; Merouane, S.; Isnard, R.; Stenzel, O.; Fischer, H.; Rynö, J.; Kissel, J.; Hilchenbach, M. (July 2021). "D/H in the refractory organics of comet 67P/Churyumov-Gerasimenko measured by Rosetta/COSIMA". Monthly Notices of the Royal Astronomical Society. 504 (4): 4940–4951. Bibcode:2021MNRAS.504.4940P. doi:10.1093/mnras/stab1028. Retrieved 15 July 2022.
- ^ Mannel, T.; Bentley, M.; Boakes, P.; Jeszenszky, H.; Ehrenfreund, P.; Engrand, C-; Koeberl, C.; Levasseur-Regourd, A.C.; Romstedt, J.; Schmied, R.; Torkar, K.; Weber, I. (October 2019). "Dust of comet 67P/Churyumov-Gerasimenko collected by Rosetta/MIDAS: classification and extension to the nanometer scale" (PDF). Astronomy & Astrophysics. 630 (A26): 14. Bibcode:2019A&A...630A..26M. doi:10.1051/0004-6361/201834851. S2CID 182330353. Retrieved 15 July 2022.
- ^ Hadraoui, K.; Cottin, H.; Ivanovski, S.; Zapf, P.; Altwegg, K.; Benilan, Y.; Biver, N.; Della Corte, V.; Fray, N.; Lasue, J.; Merouane, S.; Rotundi, A.; Zakharov, V. (October 2019). "Distributed glycine in comet 67P/Churyumov-Gerasimenko" (PDF). Astronomy & Astrophysics. 630 (A32): 8. Bibcode:2019A&A...630A..32H. doi:10.1051/0004-6361/201935018. S2CID 195549622. Retrieved 15 July 2022.
- ^ Pestoni, B.; Altwegg, K.; Balsiger, H.; Hänni, N.; Rubin, M.; Schroeder, I.; Schuhmann, M.; Wampfler, S. (January 2021). "Detection of volatiles undergoing sublimation from 67P/Churyumov-Gerasimenko coma particles using ROSINA/COPS. I. The ram gauge" (PDF). Astronomy & Astrophysics. 645 (A36): A38. Bibcode:2021A&A...645A..38P. doi:10.1051/0004-6361/202039130. Retrieved 15 July 2022.
- ^ Szopa, C.; Gomes, R.; Raulin, F.; Sternberg, R.; Coscia, D.; Cabane, M.; Meierhenrich, U.; Gautier, T.; Goesmann, F.; and the Cosac Team (May 2014). "Molecular characterization of a cometary nucleus composition with the gas chromatograph-mass spectrometer of the COSAC experiment onboard the Philae lander of the Rosetta mission" (PDF). EGU General Assembly 2014, Held 27 April 2 May 2014 in Vienna, Austria. id.12830: 12830. Bibcode:2014EGUGA..1612830S. Retrieved 15 July 2022.
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