1356:
570:
783:(MCP) behind the central focusing grid. LDEX has a sensitive area of 0.012 m. 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 20–100 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. From this data it was found that approximately 40 μm/Myr of
144:
401:
1023:
136:
20:
255:
274:
solar flare track densities), so spacecraft measurements by the
Pegasus satellites were used to determine the interplanetary dust flux, specifically the crater production flux at 100 μm size. The flux of smaller meteoroids was found to be smaller than the observed cratering flux on the lunar surface due to fast ejecta from impacts of bigger meteoroids. The flux was adjusted using data from the HEOS-2 and Pioneer 8/9 space probes.
305:
1176:
1276:. IDEX is a large-area (0.07 m) 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 operated at University of Colorado to collect impact ionization mass spectra for a range of dust samples of known composition. Its launch is planned for 2025.
1196:(CDA). A Dust Trajectory Sensor consists of four planes of parallel position sensing wire electrodes. Dust accelerator tests show that dust trajectories can be determined to an accuracy of 1% in velocity and 1° in direction. The second element of a Dust Telescope is a Large-area Mass Analyzer: a reflectron type time-of-flight mass analyzer with a sensitive area of up to 0.2 m and a mass resolution
1092:≈ 250. Besides the positive ion mode, CIDA has also a negative ion mode for better sensitivity for organic molecules. The 75 spectra obtained during the comet flybys indicate a dominance of organic matter; sulfur ions were also detected in one spectrum. In the 45 spectra obtained during the cruise phase favorable for the detection of interstellar particles, derivates of
760:
5259:
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,
593:
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, the instrument was deselected
345:
and 3.3 AU from the sun. This way, the heliocentric radial profile was determined, and shown to vary by a factor of about 100 over that distance. The
Asteroid Meteoroid Detector (AMD) on Pioneer 10 and Pioneer 11 used the optical detection and triangulation of individual meteoroids to get information
3025:
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
433:
interplanetary spacecraft carried 234 pressurized cell detectors each, mounted on the back of the main dish antenna. The stainless-steel wall thickness was 25 microns on
Pioneer 10, and 50 microns on Pioneer 11. The two instruments characterized the meteoroid environment in the outer Solar System as
420:
satellites. Each satellite carried more than 200 individual gas-filled pressurized cells with metal walls of 25 and 50 microns thick. A puncture of a cell by a meteoroid impact could be detected by a pressure sensor. These instruments provided important measurements of the near-Earth meteoroid flux.
533:
shield. Mounted on the front dust shield were three piezoelectric momentum sensors of the Dust Impact
Detection System (DIDSY). A fourth momentum sensor was mounted on the rear shield. These microphone detectors, together with other detectors, measured the dust distribution within the inner coma of
4317:
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
3874:
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,
119:
satellites carried simple 0.001 m sized microphone dust detectors in order to detect impacts of micron sized meteoroids. The obtained fluxes were orders of magnitude higher than those estimated from zodiacal light measurements. However, the latter determination had big uncertainties in the assumed
5688:
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.;
664:
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 on a single channel. The first successful dust detector in interplanetary space at about 1 AU was flown on the
273:
analyses. The craters ranged in size from 10 to 10 m, and were correlated to the mass of meteoroids based on impact simulations. The impact speed onto the lunar surface was assumed to be 20 km/s. The age of the rocks on the surface could not be determined through traditional methods (counting the
445:
rocket into near-Earth orbit. Each satellite carried 416 individual meteoroid detectors with a total detection surface of about 200 m. The detectors consisted of aluminum penetration sheets of various thicknesses: 171 m of 400 micron-thick, 16 m of 200 micron-thick, and 7.5 m of 40 micron-thick.
1264:
in cooperation with von
Hoerner & Sulger GmbH (vH&S) company. DDA will analyze interstellar and interplanetary dust on cruise to Phaethon and will study its dust environment during the encounter; of particular interest is the proportion of organic matter. Its launch is planned for 2024.
701:
spacecraft, and the LDEX detectors on the LADEE mission. The hemispherical target of 0.01 m 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
1400:
found in primitive meteorites that were transported to cold nebular regions. During March–May 2000 and July–December 2002, the spacecraft was in a favorable position to collect interstellar dust on the back side of the sample collector. Once the sample capsule was returned in
January 2006, the
1166:
within 175 km from the surface, CDA discovered active ice geysers. Detailed compositional analyses found salt-rich water ice grains close to
Enceladus, which led to the discovery of large reservoirs of liquid water oceans below the icy crust of the moon. Analyses of interstellar grains at
6536:
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)
1343:
showed that micrometeoroids smaller than a critical size (~100 micrometers) are decelerated at altitudes above 100 km slowly enough to radiate their frictional energy away without melting. Such micrometeorites sediment through the atmosphere and ultimately deposit on the ground. The most
5403:
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).
474:
films. This material responds to dust impacts by generating electrical charge due to impact cratering or penetration. Since PVDF detectors are also sensitive to mechanical vibrations and energetic particles, detectors using PVDF work acceptably well as high-rate dust detectors in very dusty
716:
were optimized for interplanetary dust measurements in the outer Solar System. The sensitive target areas were increased ten-fold to 0.1 m 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
5402:
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.;
4356:
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).
2076:
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).
186:(LASP) in Boulder, Colorado. The LASP dust accelerator facility has been 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.
601:
flythrough of the Saturn system, PWS detected intense impulse noise centered on the ring plane at 2.88 Saturn radii distance, slightly outside of the G ring. This noise was attributed to micron sized particles hitting the spacecraft. In-situ dust detections by the
3875:
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).
3773:
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).
1003:. The instruments could record up to 500 impacts per second. During comet flybys, the instruments recorded an abundance of small particles of mass less than 10 grams. Besides unequilibrated silicates, many of the particles were rich in light elements such as
5689:
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).
3628:
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).
1425:
in November 2005, picked up surface samples, and returned to Earth in June 2010. Despite some problems during sample collection, thousands of 10–100 micron sized particles were collected and are available for research in the laboratories. The second
1188:. It 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. The latter is based on the successful measurement of the dust electric charge by
5033:
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).
221:
determined a much lower flux of 100 micron sized particles that would not pose a significant hazard to the crewed Apollo missions. The first reliable dust detections of micron sized meteoroids were obtained by the dust detectors on board the
1401:
collector trays were inspected and thousands of grains from Comet Wild 2 and seven probable interstellar grains were identified. These grains are available for teaching and research from the NASA Astromaterials Curation Office.
641:
Though plasma wave instruments on various spacecraft claimed to detect dust, it was only in 2021 that a model for the generation of signals on plasma wave antennas by dust impacts was presented, based on dust accelerator tests.
5784:
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).
1344:
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.
120:
size and heliocentric radial dust density distributions. Thermal studies in the lab with microphone detectors suggested that the high count-rates recorded were due to noise generated by temperature variations in Earth orbit.
1057:
at a distance of 181 km with a speed of 10.9 km/s. During the interplanetary cruise between the comet encounters, there were favorable opportunities to analyze the interstellar dust stream discovered earlier by
1087:
missions. The impact target peeks out to the side of the spacecraft while the main part of the instrument is protected from the high-speed dust. It has a sensitive area of approximately 100 cm and a mass resolution
810:
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 in the compositional and physical properties of
1030:
spacecraft. Dust particles hitting the target at the top release ions that are pulled into the drift tube and to the reflector (bottom), where their trajectories are deflected into the ion detector (left cubic
450:
capacitor detectors that recorded penetrations of the overlying sheet. The results showed that the meteoroid hazard is significant and meteoroid protection methods must be implemented for large space vehicles.
5909:
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).
3373:
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).
193:
dust detectors, and meteor studies. 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, at
751:
identified a flow of interstellar dust sweeping through the Solar System and hyper-velocity streams of nano-dust which are emitted from Jupiter and then couple to the solar magnetic field. In addition, the
1179:
Schematic diagram of a Dust Telescope consisting of a Dust Trajectory Sensor (top part) and a Compositional Analyzer (lower part). Trajectories of ions from a dust impact onto the chemical analyzer are
346:
on their sizes and trajectories. Unfortunately, the trigger threshold was set too low, and noise corrupted the data. Zodiacal light observations at visible light wavelengths use the light scattered by
174:
The workhorse for hypervelocity dust impact experiments is the electrostatic dust accelerator. Nanometer to micrometer sized conducting dust particles are electrically charged and accelerated by an
825:(Ecliptic and South sensor) with a total target area of about 0.01 m. One sensor was shielded by the spacecraft rim from direct sunlight, whereas the other sensor was protected by a thin aluminized
7270:
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).
262:
Microcraters on lunar samples provide an extensive record of impacts onto the lunar surface. Uneroded glass splashes from big impacts covering crystalline lunar rocks preserve microcraters well.
899:
46:, as well as the potential hazards posed by these particles to spacecraft and other space-borne assets. The measurement of space dust requires the use of advanced scientific techniques such as
4475:
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).
1233:
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. The launch of the
1200:> 150. It consists of a circular plate target with the ion detector behind the center hole. In front of the target is an acceleration grid. Ions generated by an impact are reflected by a
392:
developed the IMEX model, which follows the evolution of cometary particles and hence allows us to determine the risk of collision at specific positions and times in the inner Solar System.
376:
IRAS sky maps showed structure in the sky brightness at infrared wavelengths. In addition to the wide, general zodiacal cloud and a broad, central asteroidal band, there were several narrow
1468:(Micro-Imaging Dust Analysis System) that investigated morphology and physical properties of micrometer-sized dust particles that were deposited on a collector plate, and the double-focus
6028:
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).
6941:"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"
5593:
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).
7505:"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"
6626:
Sternovsky, Z.; Mikula, R.; Horanyi, M.; Hillier, J.; Srama, R.; Postberg, F. (December 2021). "Laboratory calibration of the Interstellar Dust Experiment (IDEX) instrument".
159:
between just a few 100 m/s and 1 km/s, whereas meteoroid speeds range from a few km/s to several 100 km/s for nanometer sized dust particles. Only experimental
242:
detectors using coincident signals from ions and electrons released upon impact. The detectors had sensitive areas of approximately 0.01 m and detected outside the Earth's
3528:
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).
1260:
meteor stream that can be observed from the ground every December. DDA development is led by Ralf Srama and colleagues from the Institute of Space Systems (IRS) at the
502:. However, in low-dust environments such as interplanetary space, this sensitivity makes the detectors susceptible to noise. Because of this, the PVDF detectors on the
365:(IRAS) mapped the sky at wavelengths of 12, 25, 60, and 100 micrometers. Between wavelengths of 12 and 60 microns, zodiacal dust was a prominent feature. Later, the
927:
577:
Most instruments on a spacecraft flying through a dense dust environment will experience effects of dust impacts. A prominent example of such an instrument was the
7220:
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).
5735:
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).
787:
is redistributed due to meteoritic bombardment. Besides a continuous meteoroid bombardment, meteoroid streams cause temporary enhancements of the ejecta cloud.
34:
refers to the study of small particles of extraterrestrial material, known as micrometeoroids or interplanetary dust particles (IDPs), that are present in the
2802:
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
357:
wavelengths than visible wavelengths. However, on the ground, most of these infrared wavelengths are blocked by atmospheric absorption bands. Therefore, most
3667:
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).
2131:
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).
573:
Plasma Wave instrument, PWS (lower red arrow). Note that the antennas are truncated in this diagram and are much longer than shown, extending out 10 meters.
258:
Interplanetary dust flux measured by early dust detectors or derived from ground-based zodiacal light observations and analysis of lunar microcrater counts.
1480:(RTOF) of ROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis) to analyze cometary gas and the volatile components of cometary particulates.
929:< 1000 kg/m) meteoroids that were shielded from entering the Ecliptic sensor. The mass spectra range from those with dominant low masses (up to 30
728:
was launched in 1989 and cruised for 6 years in interplanetary space between Venus’ and Jupiter's orbit and measured interplanetary dust. The 370 kg
6464:
5457:
Hillier, J.; Green, E.; McBride, N.; Altobelli, N.; Postberg, F.; Kempf, S.; Schwanenthal, J.; Srama, R.; McDonnell, J.A.M.; Grün, E. (October 2007).
7503:
Szopa, C.; Gomes, R.; Raulin, F.; Sternberg, R.; Coscia, D.; Cabane, M.; Meierhenrich, U.; Gautier, T.; Goesmann, F.; and the Cosac Team (May 2014).
994:
350:
particles, which constitute only a few percent of the incoming light. The remainder (over 90%) is absorbed and reradiated at infrared wavelengths.
826:
38:. These particles are typically of micrometer to sub-millimeter size and are composed of a variety of materials including silicates, metals, and
901:. There was an excess of impacts recorded by the South sensor compared to the Ecliptic sensor. On the basis of the penetration studies with the
721:
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-ton
1457:
carried a suite of miniaturized sophisticated lab instruments to study collected cometary dust particles. Among them was the high-resolution
688:
233:
3482:
Kempf, S.; Beckmann, U.; Moragas-Klostermeyer, G.; Postberg, F.; Srama, R.; Economou, T.; Schmidt, J.; Spahn, F.; Grün, E. (February 2008).
1229:
mission is being developed by Sacha Kempf and colleagues at LASP. SUDA will collect spatially resolved compositional maps of Jupiter's moon
829:
from intense solar radiation. These Micrometeoroid Analyzers were calibrated with a wide range of materials at the dust accelerators of the
6406:(PDF). S. Kempf, N. Altobelli, C. Briois, E. Grün, M. Horanyi, F. Postberg, J. Schmidt, R. Srama, Z. Sternovsky, G. Tobie, and M. Zolotov.
5972:
Grün, E.; Krüger, H.; Srama, R.; Auer, S.; Colangeli, L.; Horanyi, M.; Whitnell, P.; Kissel, J.; Landgraf, M.; Svedhem, H. (October 2000).
2639:
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).
1205:
183:
1269:
6274:
Sternovsky, Z.; Grün, E.; Drake, K.; Xie, J.; Horanyi, M.; Srama, R.; Kempf, S.; Postberg, F.; Mocker, A.; Auer, S.; Krüger, H. (2011).
316:
6794:
Lunar Science Conference, 8th, Houston, Tex., March 14–18, 1977, Proceedings Volume 1. (A78-41551 18-91) New York, Pergamon Press, Inc
1453:
from August 2014 to September 2016. During this time, Rosetta's instruments analyzed the nucleus, dust, gas, and plasma environments.
796:
1489:
978:
830:
179:
308:
COBE/DIRBE 25 micron wavelength map of the sky in ecliptic coordinates. The narrow curved line at the right is the galactic plane.
7446:"Detection of volatiles undergoing sublimation from 67P/Churyumov-Gerasimenko coma particles using ROSINA/COPS. I. The ram gauge"
171:
containing dust particles, high speed dust projectiles can be used for impact cratering and dust sensor calibration experiments.
6236:
Srama, R.; Kempf, S.; Moragas-Klostermeyer, G.; Landgraf, M.; Helfert, S.; Sternovsky, Z.; Rachev, M.; Grün, E. (January 2007).
2298:
Thomas, E.; Simolka, J.; DeLuca, M.; Horanyi, M.; Janches, D.; Marshall, R; Munsat, T.; Plane, J.; Sternovski, Z. (March 2017).
6500:
5503:
Altobelli, N.; Kempf, S.; Landgraf, M.; Srama, R.; Dikarev, V.; Krüger, H.; Moragas-Klostermeyer, G.; Grün, E. (October 2003).
366:
1461:
COSIMA (Cometary Secondary Ion Mass Analyzer) that analyzed the rocky and organic composition of collected dust particles, an
1154:
completed 292 orbits around Saturn (2004–2017) and measured several million dust impacts which characterize dust primarily in
123:
An excellent review of the early days of space dust research was given by Fechtig, H., Leinert, Ch., and Berg, O. in the book
6295:
6005:
2899:
1863:
1821:
653:
detectors are the most successful dust detectors in space. With these detectors, the interplanetary dust environment between
1397:
55:
6352:
Srama, R.; Sternovsky, Z.; Kempf, S.; Horanyi, M.; Postberg, F.; Krüger, H.; Kobayashi, M.; Sterken, V. (September 2021).
2252:
Grün, E.; Fechtig, H.; Hanner, M.; Kissel, J.; Lindblad, B.A.; Linkert, D.; Maas, D.; Morfill, G.E.; Zook, H. (May 1992).
1114:. CDA is a large-area (0.1 m total sensitive area) multi-sensor dust instrument that includes a 0.01 m medium resolution (
7324:"Dust of comet 67P/Churyumov-Gerasimenko collected by Rosetta/MIDAS: classification and extension to the nanometer scale"
1521:
503:
167:, JSC) reach projectile speeds of several km/s up to 10 km/s in the laboratory. By exchanging the projectile with a
7383:; Benilan, Y.; Biver, N.; Della Corte, V.; Fray, N.; Lasue, J.; Merouane, S.; Rotundi, A.; Zakharov, V. (October 2019).
7271:
7221:
2965:"The Asteroid Belt: Doubts about the Particle Concentration Measured with the Asteroid/Meteoroid Detector on Pioneer 10"
844:
178:
to speeds up to 100 km/s. Currently, operational dust accelerators exist at IRS in Stuttgart, Germany (formally at
139:
The 3 MeV dust accelerator facility at the Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder
3204:
Soja, R.; Grün, E.; Srama, R.; Sterkem, V.; Vaubaillon, J.; Krüger, H.; Sommer, M.; Herzog, J.; Hornig, A.; Bausch, L.
1526:
1506:
1465:
706:
175:
693:
dust detector was the first detector that employed a hemispherical geometry, like all the subsequent detectors of the
7096:
3205:
7566:
6136:
Xie, J.; Sternovsky, Z.; Grün, E.; Auer, S.; Duncan, N.; Drake, K.; Le, H.; Horanyi, M.; Srama, R. (October 2011).
1119:
1019:. This suggests that most particles consisted of a predominantly chondritic core with a refractory organic mantle.
969:. These spacecraft flew by the comet at a distance of 600–1,000 km with a speed of 70–80 km/s. The PUMA (
2878:. Interplanetary Dust and Zodiacal Light. Lecture Notes in Physics. Vol. 48. Berlin, Heidelberg. p. 24.
296:, the instrument trays were analyzed. The results generally confirmed the earlier analysis of lunar microcraters.
1955:
1458:
799:
was the in-situ instrument to analyze the composition of cosmic dust. In 1974, the instrument was carried by the
635:
384:
showed that at least 80% of all Jupiter family comets had trails. When the Earth passes through a comet trail, a
282:
47:
4882:
Krüger, H.; Strub, P.; Sommer, M.; Altobelli, N.; Kimura, H.; Lohse, A.K.; Grün, E.; Srama, R. (November 2020).
1376:
at a distance of 237 km with a relative velocity of 6.1 km/s. Its dust collector consisted of 0.104 m
7319:
3230:
2798:"Impact cratering from LDEF's 5.75-year exposure: decoding of the interplanetary and earth-orbital populations"
1209:
1146:
dust streams. A highlight was the detection of electrical dust charges in interplanetary space and in Saturn's
546:
3631:"The dust distribution within the inner coma of comet P/Halley 1982i - Encounter by Giotto's impact detectors"
1167:
Saturn's distance suggest magnesium-rich grains of silicate and oxide composition, some with iron inclusions.
285:
exposed several passive impact collectors (each a few square meters in area) to the space dust environment in
7222:"The detection of solid phosphorus and fluorine in the dust from the coma of comet 67P/Churyumov-Gerasimenko"
5300:
4477:"The Lunar Dust Experiment (LDEX) Onboard the Lunar Atmosphere and Dust Environment Explorer (LADEE) Mission"
1450:
1268:
The Interstellar Dust Experiment (IDEX), developed by Mihaly Horanyi and colleagues at LASP, will fly on the
6894:
4884:"Helios spacecraft data revisited: detection of cometary meteoroid trails by following in situ dust impacts"
3344:
3151:
Reach, W.T.; Kelley, M.S.; Sykes, M. (November 2007). "A survey of debris trails from short-period comets".
2873:
6652:; Asphaug, E. (August 2001). "Origin of the Moon in a giant impact near the end of the Earth's formation".
5204:"The organic component in dust from comet Halley as measured by the PUMA mass spectrometer on board Vega 1"
4838:"Orbital and physical characteristics of micrometeoroids in the inner solar system as observed by Helios 1"
1985:"The Hypervelocity Impact Facility at the University of Kent: Recent Upgrades and Specialized Capabilities"
270:
6191:
5973:
4014:
3922:
3876:
3298:
2875:
Pioneer 10 observations of zodiacal light brightness near the ecliptic: Changes with heliocentric distance
151:
A dust accelerator is a critical facility to develop, test, and calibrate space dust instruments. Classic
7571:
7072:
4951:"A new look into the Helios dust experiment data: presence of interstellar dust inside the Earth's orbit"
4837:
4791:
4745:
4180:
3829:
3106:
2640:
2300:"Experimental setup for the laboratory investigation of micrometeoroid ablation using a dust accelerator"
1511:
1292:
for dust science was that they provided a meteoroid impact cratering record. Even more important are the
780:
199:
5261:
1130:(PVDF) detectors with sensitive areas of 0.005 m and 0.001 m, respectively. During its 6-year cruise to
97:
Even sub-millimeter sized meteoroids hitting spacecraft at speeds around 300 m/s (much faster than
42:. The study of space dust is important as it provides insight into the composition and evolution of the
7576:
7546:
6082:
Auer, S.; Grün, E.; Kempf, S.; Srama, R.; Srowig, A.; Sternovsky, Z.; Tschernjawski, V. (August 2008).
5978:
American Astronomical Society, DPS Meeting #32, Id.26.16; Bulletin of the American Astronomical Society
3484:"The E ring in the vicinity of Enceladus. I. Spatial distribution and properties of the ring particles"
687:
on eccentric orbits, it detected dust on hyperbolic orbits—that is, dust leaving the Solar System. The
553:
mission, the Mercury Dust Monitor (MDM) will measure the dust environments of interplanetary space and
370:
6353:
5595:"Cassini between Earth and asteroid belt: first in-situ charge measurements of interplanetary grains"
1135:
735:
was launched a year later and went on a direct trajectory to Jupiter, which it reached in 1992 for a
87:
7504:
3968:
206:
under visual control. This way, a wide range of dust materials could be accelerated to high speeds.
6403:
5690:
5643:
4272:
4060:
3630:
2518:
2407:
2207:
2133:"3 MV hypervelocity dust accelerator at the Colorado Center for Lunar Dust and Atmospheric Studies"
1693:
1380:
and 0.015 m aluminium foil; one side of the detector was exposed to the flow of cometary dust. The
1368:
was the first mission to return samples from a comet and from interstellar space. In January 2004,
631:
539:
388:
is observed from the ground. Due to the enhanced risk to spacecraft in such meteoroid streams, the
4529:
Horanyi, M.; Szalay, J.; Kempf, S.; Schmidt, J.; Grün, E.; Srama, R.; Sternovsky, Z. (June 2015).
3079:
7561:
7444:; Balsiger, H.; Hänni, N.; Rubin, M.; Schroeder, I.; Schuhmann, M.; Wampfler, S. (January 2021).
5911:
5848:
5786:
5594:
5545:
5458:
5404:
4707:
4412:
4358:
3775:
3668:
3583:
3529:
3483:
3429:
3376:"Dust counter and mass analyser (DUCMA) measurements of comet Halley's coma from Vega spacecraft"
3375:
2928:
Physical Studies of Minor Planets, Proceedings of IAU Colloq. 12, Held in Tucson, AZ, March, 1971
2689:
2353:
2299:
2253:
2132:
2078:
1845:
1739:
1547:
1462:
1313:
1261:
1245:
1213:
1127:
558:
381:
51:
7318:
Mannel, T.; Bentley, M.; Boakes, P.; Jeszenszky, H.; Ehrenfreund, P.; Engrand, C-; Koeberl, C.;
2835:
1801:
763:
Cut-through view of the Lunar Dust Experiment (LDEX) on LADEE, for dust detection in lunar orbit
23:
Small glassy lunar sample peppered with microcraters. The central pits are surrounded by bright
7445:
7384:
7323:
5544:
Postberg, F.; Kempf, S.; Srama, R.; Green, S.; Hillier, J-; McBride, N.; Grün, E. (July 2006).
4883:
4226:
2607:
In: Lunar and Planetary Science Conference, 10th, Houston, Tex., March 19–23, 1979, Proceedings
666:
467:
404:
Panel of 18 pressurized cells mounted on the back of the main dish antenna of Pioneer 10 and 11
290:
223:
7272:"D/H in the refractory organics of comet 67P/Churyumov-Gerasimenko measured by Rosetta/COSIMA"
6789:
6237:
6029:
4950:
4476:
2797:
2602:
2564:
1639:
1601:
1204:
shaped grid onto the center ion detector. Prototypes of dust telescope have been built at the
373:
provided a complete high-precision survey of the zodiacal dust cloud at the same wavelengths.
86:
from several positions on the ground, the trajectory and the entry speed can be determined by
7556:
3921:
Gurnett, D.A.; Kurth, W.S.; Scarf, F.K.; Burns, J.A.; Cuzzi, J.N.; Grün, E. (December 1987).
1516:
1364:
1340:
1220:
1037:
612:
578:
490:
389:
7474:
7403:
7342:
7088:
7005:
6956:
6560:
6045:
5706:
5659:
4969:
4912:
4853:
4807:
4761:
4641:
4288:
4196:
3923:"Micron-sized particle impacts detected near Uranus by the Voyager 2 plasma wave instrument"
3892:
3646:
2851:
2656:
2534:
2423:
2223:
1709:
1492:
COSAC experiment to analyze organic molecules in the comet's atmosphere and on its surface.
985:. Dust particle hitting the small (approximately 5 cm) impact target generated ions by
7551:
7515:
7470:
7399:
7338:
7283:
7132:
7076:
7001:
6952:
6906:
6865:
6801:
6742:
6661:
6631:
6556:
6361:
6249:
6203:
6149:
6095:
6041:
5985:
5923:
5860:
5798:
5748:
5702:
5655:
5606:
5557:
5516:
5470:
5416:
5353:
5341:
5315:
5273:
5218:
5203:
5161:
5146:
5104:
5047:
5015:
4965:
4908:
4849:
4803:
4757:
4719:
4653:
4604:
4542:
4488:
4434:
4370:
4327:
4284:
4238:
4192:
4136:
4082:
4026:
3980:
3967:
Gurnett, D.A.; Kurth, S.W.; Granroth, L.J.; Allendorf, S.C.; Poynter, R.L. (October 1991).
3934:
3888:
3841:
3787:
3680:
3642:
3595:
3541:
3495:
3441:
3387:
3310:
3272:
3170:
3118:
3045:
2976:
2935:
2879:
2847:
2809:
2747:
2735:
2701:
2652:
2614:
2576:
2530:
2492:
2419:
2365:
2311:
2265:
2219:
2144:
2090:
2029:
1909:
1851:
1751:
1705:
1651:
1613:
1559:
1501:
1445:
1348:
first reliably identified the extraterrestrial nature of collected dust particles by their
1328:. These samples are available for research and teaching projects. From 1970 to 1976, three
1193:
1100:
912:
834:
608:
604:
485:
195:
164:
91:
506:
also needed shielded reference detectors in order to determine the background noise rate.
494:
mission, the Dust Flux Monitor Instrument (DFMI) used PVDF detectors to study dust in the
8:
5912:"Flux and composition of interstellar dust at Saturn from Cassini's Cosmic Dust Analyzer"
5849:"A salt-water reservoir as the source of a compositionally stratified plume on Enceladus"
1485:
1440:
were returned. JAXA shares about 10% of the collected samples with NASA sample curation.
1104:
964:
684:
481:
438:
347:
320:
215:
203:
79:
7519:
7287:
7136:
7080:
6918:
6910:
6869:
6805:
6746:
6665:
6635:
6404:
SUDA: A Dust Mass Spectrometer for Compositional Surface Mapping for a Mission to Europa
6365:
6253:
6242:
Workshop on Dust in Planetary Systems (ESA SP-643). September 26–30, 2005, Kauai, Hawaii
6207:
6153:
6099:
5989:
5927:
5864:
5802:
5752:
5610:
5561:
5520:
5474:
5420:
5357:
5319:
5277:
5222:
5165:
5108:
5051:
5019:
4723:
4657:
4608:
4546:
4492:
4438:
4374:
4331:
4242:
4140:
4086:
4030:
3984:
3938:
3845:
3791:
3684:
3599:
3545:
3499:
3445:
3391:
3314:
3276:
3174:
3122:
3049:
2980:
2939:
2883:
2813:
2751:
2705:
2618:
2580:
2496:
2369:
2315:
2269:
2148:
2094:
2033:
1913:
1855:
1755:
1655:
1617:
1563:
7460:
7415:
7354:
7233:
7150:
7019:
6970:
6790:"Interplanetary dust: a new source of extraterrestrial material for laboratory studies"
6765:
6730:
6685:
6572:
6546:
6379:
6301:
6057:
5947:
5884:
5822:
5766:
5432:
5377:
5234:
5177:
5120:
5063:
4981:
4924:
4898:
4676:
4622:
4566:
4504:
4450:
4424:
4386:
4098:
4072:
3803:
3696:
3557:
3403:
3186:
3160:
3061:
3035:
2992:
2771:
2454:"Pegasus satellite measurements of meteoroid penetration /February 16 - July 20, 1965/"
1937:
1899:
1775:
1667:
1575:
1355:
1345:
1066:
1049:
at a distance of 240 km with a relative speed of 6.1 km/s. In February 2011,
729:
722:
358:
266:
6826:
5997:
5787:"Cassini Dust Measurements at Enceladus and Implications for the Origin of the E Ring"
4446:
2923:
2079:"A 2 MV Van de Graaff accelerator as a tool for planetary and impact physics research"
7419:
7358:
7154:
7092:
6974:
6965:
6940:
6770:
6677:
6576:
6383:
6291:
6165:
6111:
6061:
6001:
5939:
5876:
5814:
5770:
5761:
5736:
5369:
5124:
5067:
4985:
4928:
4861:
4815:
4769:
4681:
4626:
4558:
4296:
4204:
4102:
3969:"Micron-size particles detected near Neptune by the Voyager 2 plasma wave instrument"
3853:
3807:
3607:
3561:
3457:
3407:
3130:
3000:
2895:
2763:
2713:
2664:
2542:
2431:
2381:
2327:
2231:
2160:
2106:
1941:
1859:
1817:
1767:
1717:
1671:
1469:
1139:
1123:
1063:
1000:
986:
948:
941:
936:), compatible with silicates, to those with dominant high masses (between 50 and 60 m
822:
816:
807:
800:
736:
650:
569:
519:
515:
342:
239:
190:
156:
7023:
6305:
5951:
5826:
5436:
5381:
4508:
4359:"Discovery of Jovian dust streams and interstellar grains by the Ulysses spacecraft"
4250:
3299:"Results of Pioneer 10 and 11 Meteoroid Experiments: Interplanetary and Near-Saturn"
3190:
3065:
2775:
1886:
Veysset, D.; Lee, J-H.; Hassani, M.; Kooi, S.; Thomas, E.; Nelson, K. (March 2021).
1779:
739:
that put the spacecraft on a heliocentric orbit of 80 degrees inclination. In 1995,
58:
to accurately characterize the physical and chemical properties of these particles.
7478:
7407:
7346:
7291:
7243:
7194:
7140:
7121:"Preliminary analysis of the Hayabusa2 samples returned from C-type asteroid Ryugu"
7084:
7009:
6960:
6914:
6873:
6760:
6750:
6689:
6669:
6590:
6564:
6369:
6283:
6211:
6157:
6103:
6049:
5993:
5931:
5888:
5868:
5806:
5756:
5710:
5663:
5642:
Kempf, S.; Beckmann, U.; Srama, R.; Horanyi, M.; Auer, S.; Grün, E. (August 2006).
5614:
5565:
5524:
5478:
5424:
5361:
5281:
5238:
5226:
5181:
5169:
5112:
5055:
4973:
4916:
4857:
4811:
4765:
4671:
4661:
4612:
4570:
4550:
4496:
4454:
4442:
4390:
4378:
4335:
4292:
4246:
4200:
4152:
4144:
4090:
4034:
3988:
3942:
3896:
3849:
3830:"Micron-sized particles detected near Saturn by the Voyager plasma wave instrument"
3795:
3700:
3688:
3603:
3549:
3503:
3449:
3395:
3345:"Pegasus satellite measurements of meteoroid penetration (Feb. 16 - July 20, 1965)"
3318:
3178:
3126:
3053:
2984:
2887:
2755:
2709:
2660:
2538:
2427:
2373:
2319:
2273:
2227:
2152:
2098:
2037:
1996:
1927:
1917:
1809:
1759:
1713:
1659:
1579:
1567:
1301:
554:
168:
39:
7482:
7411:
7350:
6137:
6083:
4920:
4124:
3828:
Gurnett, D.A.; Grün, E.; Gallagher, D.; Kurth, W.S.; Scarf, F.L. (February 1983).
2017:
1763:
1602:"The distribution of small interplanetary dust particles in the vicinity of Earth"
7441:
7380:
5618:
5569:
5482:
4977:
4015:"Dust particles detected near Giacobini-Zinner by the ICE Plasma Wave Instrument"
3747:
3721:
3553:
3507:
3182:
2988:
2759:
2565:"12054 and 76215: new measurements of interplanetary dust and solar flare fluxes"
2001:
1984:
1437:
1389:
1385:
1155:
838:
743:
started its 7-year path through the Jovian system with several flybys of all the
495:
286:
98:
1813:
1436:
in June 2018. About 5 g of surface and sub-surface material from this primitive
408:
In the early 1960s, pressurized cell micrometeorite detectors were flown on the
7145:
7120:
6735:
Proceedings of the National Academy of Sciences of the United States of America
6703:
6275:
6215:
5089:
3799:
3776:"Mercury Dust Monitor (MDM) Onboard the Mio Orbiter of the BepiColombo Mission"
3669:"Dust particle impacts during the Giotto encounter with comet Grigg-Skjellerup"
1477:
1329:
1317:
1293:
1273:
1225:
1185:
1071:
997:
819:
812:
784:
744:
594:
and, hence, no dedicated dust instrument was carried by either Voyager 1 or 2.
526:
312:
71:
6852:
Tsou, P.; Brownlee, D. E.; Sandford, S. A.; Horz, F.; Zolensky, M. E. (2003).
6568:
6287:
6053:
5714:
5667:
5428:
4746:"The ion-composition of the plasma produced by impacts of fast dust particles"
4593:"Lunar meteoritic gardening rate derived from in situ LADEE/LDEX measurements"
4530:
4500:
3900:
3260:
2891:
2519:"First results of the micrometeoroid experiment s 215 on the HEOS 2 satellite"
2480:
2453:
2408:"The ion-composition of the plasma produced by impacts of fast dust particles"
1548:"Direct Measurement of Interplanetary Dust Particles in the Vicinity of Earth"
7540:
7296:
7248:
2185:
1422:
1253:
1230:
1147:
930:
385:
243:
160:
143:
83:
5935:
5810:
5365:
4666:
4225:
Dietzel, G; Fechtig, H.; Grün, E.; Hoffmann, H.J.; Kissel, J. (March 1973).
4157:
4059:
Shen, M.M.; Sternovsky, Z.; Garzelli, Â.; Malaspina, D.M. (September 2021).
4038:
3946:
3322:
2736:"A Direct Measurement of the Terrestrial Mass Accretion Rate of Cosmic Dust"
2569:
Lunar Science Conference, 8th, Houston, Tex., March 14–18, 1977, Proceedings
6895:"The Stardust Mission: Analyzing Samples from the Edge of the Solar System"
6774:
6755:
6681:
6358:
15th Europlanet Science Congress 2021, Held Virtually, 13–24 September 2021
6169:
6115:
5943:
5880:
5818:
5373:
5035:
4685:
4562:
4339:
3461:
3004:
2767:
2603:"Properties of microcraters and cosmic dust of less than 1000 Å dimensions"
2385:
2331:
2164:
2110:
1771:
1433:
1333:
400:
90:. Atmospheric entry speeds of up to 72,000 m/s have been observed for
43:
35:
5847:
Postberg, F.; Schmidt, J.; Hillier, J.; Kempf, S.; Srama, R. (June 2011).
1022:
7168:
6878:
6853:
6649:
6482:
6420:
6374:
5529:
5504:
5285:
4617:
4592:
4429:
4094:
3481:
3040:
1932:
1312:
compositions, important conclusions can be drawn, such as concerning the
718:
416:
410:
67:
5872:
4554:
189:
Dust accelerators are used for impact cratering studies, calibration of
135:
7064:
7063:
Bottke, William F.; DeMeo, Francesca E.; Michel, Patrick, eds. (2015).
7014:
6989:
6326:
5301:"Mass-spectrometric Measurements of Dust at Comets Wild-2 and Tempel-1"
2996:
2964:
2277:
2062:
1663:
1473:
1352:. These stratospheric dust samples are available for further research.
1325:
1289:
1201:
982:
940:), compatible with iron and molecular ions. Meteoroid streams and even
429:
423:
337:
331:
315:
observations at different heliocentric distances were performed by the
109:
103:
24:
7512:
EGU General Assembly 2014, Held 27 April 2 May 2014 in Vienna, Austria
6235:
6161:
6107:
4148:
3992:
3453:
2377:
2323:
2156:
2102:
2041:
1922:
1887:
265:
The number of microcraters was measured on a single rock sample using
6731:"The Theory of Micro-Meteorites. Part I. In an Isothermal Atmosphere"
6673:
6410:
Vol. 9, EPSC2014-229, 2014. European Planetary Science Congress 2014.
5687:
5230:
5173:
5116:
5059:
5036:"Composition of comet Halley dust particles from Giotto observations"
4382:
4061:"Electrostatic Model for Antenna Signal Generation From Dust Impacts"
3873:
3692:
3399:
2795:
1571:
1428:
1393:
1349:
1321:
1285:
1249:
1163:
589:
583:
115:
75:
6990:"Final reports of the Stardust Interstellar Preliminary Examination"
5308:
EPSC-DPS Joint Meeting 2011, Held 2–7 October 2011 in Nantes, France
3430:"Polyvinylidene fluoride dust detector response to particle impacts"
1640:"Solid Component of Interplanetary Matter from Vehicle Observations"
1035:
The Cometary and Interstellar Dust Analyzer (CIDA) was flown on the
254:
19:
7465:
7322:; Romstedt, J.; Schmied, R.; Torkar, K.; Weber, I. (October 2019).
7238:
6628:
AGU Fall Meeting 2021, Held in New Orleans, LA, 13–17 December 2021
6551:
5459:"Interplanetary dust detected by the Cassini CDA Chemical Analyser"
5090:"Composition of comet Halley dust particles from Vega observations"
4903:
4640:
Szalay, J.; Pokorny, P.; Jenniskens, P.; Horanyi, M. (March 2018).
4077:
4013:
Gurnett, D.A.; Averkamp, T.F.; Scarf, F.L.; Grün, E. (March 1986).
3057:
1904:
1808:. Astronomy and Astrophysics Library. Springer,com. pp. 1–55.
1413:
1405:
1373:
1305:
1257:
1054:
1046:
1012:
1004:
499:
442:
354:
147:
Typical projectile size and speed performances of dust accelerators
4744:
Dalmann, B.K.; Grün, E.; Kissel, J.; Dietzel, H. (February 1977).
3165:
2872:
Hanner, M.S.; Sparrow, J.G.; Weinberg, J.L.; Beeson, D.E. (1976).
2517:
Hoffmann, H.J.; Fechtig, H.; Grün, E.; Kissel, J. (January 1975).
304:
299:
6854:"Wild 2 and interstellar sample collection and Earth return"
5505:"Cassini between Venus and Earth: Detection of interstellar dust"
5342:"The Cometary and Interstellar Dust Analyzer at Comet 81P/Wild 2"
2641:"Lunar microcraters: Implications for the micrometeoroid complex"
2018:"Electrostatic Acceleration of Microparticles to Hypervelocities"
1377:
1309:
1297:
1143:
1093:
906:
658:
624:
7037:
6446:
5299:
Kissel, J.; Makinen, T.; Schmidt, W.; Silen, J. (October 2011).
1175:
557:. MDM is composed of four piezoelectric ceramic sensors made of
5734:
5262:"Cometary and Interstellar Dust Analyzer for comet Wild 2"
4706:
Grün, E.; Fechtig, H.; Gammelin, P.; Kissel, J (October 1975).
4411:
Krüger, H.; Krivov, A.V.; Sremsevic, M.; Grün, E. (July 2003).
4058:
3666:
2208:"Impact phenomena of micrometeorites on lunar surface material"
2206:
Neukum, G.; Mehl, A.; Fechtig, H.; Zähringer, J. (March 1970).
1384:
cometary samples were a mix of different components, including
1131:
1111:
1083:
1077:
1016:
1008:
959:
953:
779:
dust detectors. The most sensitive impact charge detector is a
620:
530:
462:
456:
6625:
5908:
5144:
4639:
4474:
3372:
2963:
Auer, S.; Soberman, R.K.; Neste, S.L.; Lichtenberg, K (1974).
2836:"On the spatial distribution of interplanetary dust near 1 AU"
1844:
Grün, E.; Gustafson, B.A.S.; Dermott, S.; Fechtig, H. (2001).
627:, dust concentrations in the equatorial planes were observed.
466:
missions were equipped with a new dust detector, developed by
7317:
6608:
6196:
Nuclear Instruments and Methods in Physics Research Section A
6190:
Rachev, M.; Srama, R.; Srowig, A.; Grün, E. (December 2004).
5340:
Kissel, J.; Krueger, F.; Silen, J.; Clark, B.C. (June 2004).
5006:
Kissel, J. (1986). "The Giotto Particulate Impact Analyser".
4413:"Impact-generated dust clouds surrounding the Galilean moons"
3966:
3206:"IMEX – Interplanetary Meteoroid Environment for eXploration"
2406:
Dalmann, B; Grün, E.; Kissel, J.; Dietzel, H. (August 1978).
1546:
McCracken, C.W.; Alexander, W.M.; Dubin, M. (November 1961).
1216:, Germany, and tested at their respective dust accelerators.
768:
756:
instrument detected ejecta clouds around the Galilean moons.
654:
476:
447:
377:
361:
observations are done from space observatory satellites. The
5456:
5145:
Jessberger, E.; Christoforidis, A; Kissel, J. (April 1988).
3627:
2962:
1983:
Hibbert, R.; Cole, M.J.; Price, M.C.; Burchel, M.J. (2017).
638:, dust impacts were observed by the plasma wave instrument.
446:
Placed behind these penetration sheets were 12 micron-thick
7439:
7378:
6351:
5846:
5502:
5258:
5147:"Aspects of the major element composition of Halley's dust"
4836:
Grün, E.; Pailer, N; Fechtig, H.; Kissel, J. (March 1980).
4642:"Activity of the 2013 Geminid meteoroid stream at the Moon"
3772:
3527:
2871:
2688:
Grün, E.; Zook, H.A.; Fechtig, H.; Giese, R.H. (May 1985).
2638:
1843:
1409:
1241:
702:
explored the Earth dust environment within 10 Earth radii.
615:
confirmed the existence of an extended G ring. Also during
561:, from which impact signals will be recorded and analyzed.
471:
362:
278:
152:
6613:
Institute for Modeling Plasma, Atmospheres and Cosmic Dust
5032:
4881:
4316:
4224:
3235:
Tracing the dust trails of Comet 67P/Churyumov-Gerasimenko
2297:
2205:
437:
In preparation for the Apollo Missions to the moon, three
7502:
7269:
6535:
5783:
5691:"In situ dust measurements in the inner Saturnian system"
5641:
5637:
5635:
5298:
4705:
4528:
4410:
4318:
Radial Traverses through the Interplanetary Dust Cloud".
3877:"In situ dust measurements in the inner Saturnian system"
3827:
2516:
1096:
were suggested as constituents of the organic component.
759:
525:
was protected from space dust by a 1 mm-thick front
7385:"Distributed glycine in comet 67P/Churyumov-Gerasimenko"
6851:
6787:
5401:
4743:
4012:
3024:
2796:
McDonnell, J.A.M.; the Canterbury LDEF MAP team (1992).
2405:
683:
detectors had sensitive target areas of 0.01 m. Besides
214:
Tennis court sized (200 m) penetration detectors on the
101:) can cause significant damage. Therefore, the early US
6518:
5902:
5592:
5543:
5339:
4835:
2481:"Reliability of cosmic dust data from Pioneers 8 and 9"
2251:
2015:
1982:
1545:
869:
857:
534:
the comet. These instruments also measured dust during
6273:
5632:
5588:
5586:
5496:
3920:
872:
860:
7219:
6938:
6788:
Brownlee, D.E.; Tomandl, D.A.; Olszewski, E. (1977).
6276:"Novel instrument for Dust Astronomy: Dust Telescope"
6189:
6135:
6027:
5728:
5537:
4948:
4310:
2075:
1885:
977:) instruments were developed by Jochen Kissel of the
915:
847:
74:
from myriads of interplanetary dust particles and as
6939:
Brownlee, D.; Joswiak, D.; Mtrajt, G. (April 2012).
6138:"Dust trajectory sensor: Accuracy and data analysis"
4949:
Altobelli, N.; Grün, E.; Landgraf, M. (March 2006).
4531:"A permanent, asymmetric dust cloud around the Moon"
4355:
3960:
3821:
2687:
7379:Hadraoui, K.; Cottin, H.; Ivanovski, S.; Zapf, P.;
5971:
5840:
5777:
5681:
5583:
5088:Kissel, J.; Sagdeev, R.Z.; et al. (May 1986).
4271:Fechtig, H.; Grün, E.; Morfill, G.E. (April 1979).
4006:
3914:
2130:
1212:, USA and at the Institute of Space Systems of the
905:film, this excess was interpreted to be due to low
841:of the mass spectra of the Helios sensors was low:
6238:"Laboratory Tests of the Large Area Mass Analyser"
6081:
4270:
4227:"The HEOS 2 and HELIOS micrometeoroid experiments"
2921:
2016:Shelton, H.; Hendricks, C.D.; Wuerker, RF (1960).
1799:
1599:
921:
894:{\displaystyle R={\cfrac {M}{\Delta M}}\approx 10}
893:
7276:Monthly Notices of the Royal Astronomical Society
7226:Monthly Notices of the Royal Astronomical Society
7062:
5741:Monthly Notices of the Royal Astronomical Society
5644:"The electrostatic potential of E ring particles"
4646:Monthly Notices of the Royal Astronomical Society
4404:
4264:
3427:
2922:Soberman, R.K.; Neste, S.I.; Petty, A.F. (1971).
2834:Leinert, C; Hanner, M.; Pitz, E (February 1978).
2833:
1396:fragments, and high-temperature condensates like
7538:
7038:"Astromaterials Acquisition and Curation Office"
3867:
3428:James, D.; Hoxie, V.; Horanyi, M. (March 2010).
3203:
3150:
2478:
1316:of the Moon's formation. From 1969 to 1972, six
1240:The DESTINY Dust Analyzer (DDA) will fly on the
947:Twin dust mass analyzers were flown on the 1986
4942:
4181:"A source for hyperbolic cosmic dust particles"
4122:
3231:"Dust trail of comet 67P/Churyumov-Gerasimenko"
2690:"Collisional balance of the meteoritic complex"
2600:
1888:"High-velocity micro-projectile impact testing"
1332:returned 301 grams of lunar material. In 2020,
1256:. Phaethon is believed to be the origin of the
300:Optical and infrared zodiacal dust observations
202:by charging dust particles by an ion beam in a
7042:Astromaterials Acquisition and Curation Office
6465:"Germany and Japan begin new asteroid mission"
5974:"Dust Telescope: A New Tool for Dust Research"
5450:
5395:
4065:Journal of Geophysical Research: Space Physics
3530:"Student Dust Counter: Status report at 38 AU"
3254:
3252:
2562:
769:Lunar Atmosphere and Dust Environment Explorer
767:The Lunar Dust Experiment (LDEX) on board the
645:
529:(1.85 m diameter) and a 12 mm-thick rear
509:
6899:Annual Review of Earth and Planetary Sciences
6084:"Characteristics of a dust trajectory sensor"
5546:"Composition of jovian dust stream particles"
5201:
5087:
4590:
4351:
4349:
2958:
2956:
2683:
2681:
2479:Grün, E.; Berg, O.E.; Dohnanyi, J.S. (1973).
1184:A Dust Telescope is an instrument to perform
989:. The instruments were high mass resolution (
790:
6988:Westphal, A.; et al. (September 2014).
6704:"Lunar Rocks and Soils from Apollo Missions"
6648:
4783:
4231:Journal of Physics E: Scientific Instruments
3588:Journal of Physics E: Scientific Instruments
2733:
2354:"Microparticle accelerator of unique design"
1800:Fechtig, H.; Leinert, Ch.; Berg, O. (2001).
1206:Laboratory for Atmospheric and Space Physics
771:(LADEE) mission is a smaller version of the
479:or planetary rings (as was the case for the
353:The zodiacal dust cloud is much brighter at
184:Laboratory for Atmospheric and Space Physics
6030:"Development of AN Advanced Dust Telescope"
4829:
4699:
3249:
3104:
2924:"Asteroid Detection from Pioneers F and G?"
1270:Interstellar Mapping and Acceleration Probe
209:
56:laser-induced breakdown spectroscopy (LIBS)
5260:N. G.; Zolensky, M. E.; Heiss, C. (2003).
4789:
4346:
2953:
2734:Love, s:g; Brownlee, D.A. (October 1993).
2678:
1740:"Some Doubts about the Earth's Dust Cloud"
1279:
7464:
7295:
7247:
7237:
7144:
7013:
6964:
6877:
6764:
6754:
6550:
6373:
5760:
5528:
4902:
4675:
4665:
4616:
4428:
4156:
4076:
3584:"The Giotto dust impact detection system"
3581:
3164:
3039:
2000:
1931:
1921:
1903:
1606:Smithsonian Contributions to Astrophysics
1600:McCracken, C.W.; Alexander, W.M. (1963).
1336:collected 1.7 kg of lunar material.
6987:
6892:
4273:"Micrometeoroids within ten Earth radii"
4178:
1691:
1637:
1354:
1174:
1021:
979:Max Planck Institute for Nuclear Physics
831:Max Planck Institute for Nuclear Physics
758:
568:
564:
399:
395:
303:
253:
180:Max Planck Institute for Nuclear Physics
142:
134:
18:
7119:Yada, T.; et al. (December 2021).
7089:10.2458/azu_uapress_9780816532131-ch021
6728:
3258:
3105:Sykes, M.; Walker, R. (February 1992).
3084:COBE Slide Set - High-Resolution Images
2451:
2445:
1737:
1272:(IMAP) in orbit about the Sun–Earth L1
944:particles were identified in the data.
470:, which used polyvinylidene difluoride
249:
7539:
5202:Kissel, J.; Krueger, F. (April 1987).
5005:
4708:"Das Staubexperiment auf Helios (E10)"
4125:"The Pioneer 8 cosmic dust experiment"
4123:Berg, O.E.; Rischardson, F.F. (1969).
3261:"The Near-Earth Meteoroid Environment"
2601:Morrison, D.A.; Clanton, U.S. (1979).
2351:
1126:detector, and two high-rate polarized
434:well as near Jupiter and near Saturn.
367:Diffuse Infrared Background Experiment
48:secondary ion mass spectrometry (SIMS)
6501:"Die neue Asteroidenmission DESTINY+"
4792:"The penetration limit of thin films"
4179:Zook, H.; Berg, O.E. (January 1975).
3296:
7118:
6354:"Dust Telescopes for Dust Astronomy"
5737:"The composition of Saturn's E ring"
5252:
4591:Szalay, J.; Horanyi, M. (May 2016).
3352:NTRS - NASA Technical Reports Server
3265:Rep. NASA Tech. Note, NASA-TN-D-3717
2458:NTRS - NASA Technical Reports Server
1490:gas chromatography–mass spectrometry
246:on average one impact per ten days.
130:
7169:"Hayabusa Asteroid Itokawa Samples"
6994:Meteoritics & Planetary Science
6945:Meteoritics & Planetary Science
6919:10.1146/annurev-earth-050212-124203
4790:Pailer, N.; Grün, E. (March 1980).
3342:
3026:of the Interplanetary Dust Cloud".
2563:Morrison, D.A.; Zinner, E. (1977).
2212:Earth and Planetary Science Letters
1522:Venetia Burney Student Dust Counter
1432:mission rendezvoused with asteroid
806:from the Earth's orbit down to 0.3
504:Venetia Burney Student Dust Counter
380:. Follow-up observations using the
13:
7195:"Hayabusa2 Asteroid Ryugu Samples"
5405:"The Cassini Cosmic Dust Analyzer"
3086:. NASA Goddard Space Flight Center
2452:Naumann, R.J. (December 1, 1965).
1963:JSC Experimental Impact Laboratory
1527:Micro-Imaging Dust Analysis System
1507:Galileo and Ulysses Dust Detectors
1170:
874:
815:. The instrument consisted of two
518:at a distance of 600 km, the
341:space probes, ranging between 0.3
238:spacecraft. Both instruments were
176:electrostatic particle accelerator
14:
7588:
1320:collected 382 kilograms of lunar
1150:. During the following 13 years,
277:From April 1984 to January 1990,
7496:
7433:
7372:
7311:
7263:
7213:
7187:
7161:
7112:
7065:"Hayabusa Sample Return Mission"
7056:
7030:
6981:
6966:10.1111/j.1945-5100.2012.01339.x
6932:
6886:
6845:
6819:
6781:
6722:
6696:
6642:
6619:
6601:
6583:
6529:
6525:. von Hoerner & Sulger GmbH.
6511:
6493:
6475:
6457:
6439:
6413:
6397:
6345:
6319:
6267:
6229:
6142:Review of Scientific Instruments
6088:Review of Scientific Instruments
5762:10.1111/j.1365-2966.2007.11710.x
4129:Review of Scientific Instruments
3722:"Mercury Magnetospheric Orbiter"
3434:Review of Scientific Instruments
3107:"Cometary dust trails I. Survey"
2358:Review of Scientific Instruments
2304:Review of Scientific Instruments
2186:"LASP dust accelerator facility"
2137:Review of Scientific Instruments
2083:Review of Scientific Instruments
1956:"Experimental Impact Laboratory"
1478:time of flight mass spectrometer
289:. After recovery of LDEF by the
6858:Journal of Geophysical Research
6519:"von Hoerner & Sulger GmbH"
6183:
6148:(10): 105104-105104-11 (2011).
6129:
6075:
6021:
5965:
5509:Journal of Geophysical Research
5333:
5292:
5266:Journal of Geophysical Research
5195:
5138:
5081:
5026:
4999:
4875:
4737:
4633:
4584:
4522:
4468:
4218:
4172:
4116:
4052:
3973:Journal of Geophysical Research
3927:Journal of Geophysical Research
3766:
3740:
3714:
3660:
3621:
3582:McDonnell, J.A.M. (June 1987).
3575:
3521:
3475:
3421:
3366:
3336:
3303:Journal of Geophysical Research
3290:
3259:Naumann, R.J. (November 1966).
3223:
3197:
3144:
3098:
3072:
3018:
2915:
2865:
2827:
2789:
2727:
2632:
2594:
2556:
2510:
2472:
2399:
2345:
2291:
2245:
2199:
2178:
2124:
2069:
2055:
2009:
1976:
1692:Elsässer, H. (September 1963).
1459:secondary ion mass spectrometer
1359:Stardust aerogel dust collector
1210:University of Colorado, Boulder
636:International Cometary Explorer
611:and camera observations of the
363:Infrared Astronomical Satellite
283:Long Duration Exposure Facility
1948:
1879:
1837:
1793:
1738:Nilsson, C. (September 1966).
1731:
1685:
1631:
1593:
1539:
1062:. CIDA is a derivative of the
797:Helios Micrometeoroid Analyzer
547:Mercury Magnetospheric Orbiter
1:
6729:Whipple, F. (December 1950).
6094:(8): 084501-084501-7 (2008).
5998:10.1016/S0964-2749(02)80341-9
4447:10.1016/S0019-1035(03)00127-1
3297:Humes, D.H. (November 1980).
2352:Vedder, J.F. (January 1978).
1764:10.1126/science.153.3741.1242
1532:
1408:samples were returned by the
1237:mission is planned for 2024.
271:scanning electron microscopic
52:atomic force microscopy (AFM)
7453:Astronomy & Astrophysics
7392:Astronomy & Astrophysics
7331:Astronomy & Astrophysics
6489:. Hoerner & Sulger GmbH.
6327:"Institute of Space Systems"
5619:10.1016/j.icarus.2004.05.017
5570:10.1016/j.icarus.2006.02.001
5483:10.1016/j.icarus.2007.03.024
5008:ESA Spec. Publ., ESA SP-1077
4891:Astronomy & Astrophysics
4862:10.1016/0032-0633(80)90022-7
4816:10.1016/0032-0633(80)90021-5
4770:10.1016/0032-0633(77)90017-4
4597:Geophysical Research Letters
4297:10.1016/0032-0633(79)90128-4
4205:10.1016/0032-0633(75)90078-1
4019:Geophysical Research Letters
3854:10.1016/0019-1035(83)90145-8
3554:10.1016/j.icarus.2018.11.012
3508:10.1016/j.icarus.2007.06.027
3183:10.1016/j.icarus.2007.03.031
3131:10.1016/0019-1035(92)90037-8
2989:10.1126/science.186.4164.650
2760:10.1126/science.262.5133.550
2714:10.1016/0019-1035(85)90121-6
2665:10.1016/0032-0633(75)90076-8
2543:10.1016/0032-0633(75)90080-X
2432:10.1016/0032-0633(77)90017-4
2232:10.1016/0012-821X(70)90095-6
2002:10.1016/j.proeng.2017.09.775
1718:10.1016/0032-0633(63)90040-0
1638:Nazarova, T.N. (July 1968).
538:'s encounter with the comet
475:environments, like cometary
7:
7483:10.1051/0004-6361/202039130
7412:10.1051/0004-6361/201935018
7351:10.1051/0004-6361/201834851
7073:University of Arizona Press
6539:Planetary and Space Science
5980:. COSPAR Colloquia Series.
5695:Planetary and Space Science
5648:Planetary and Space Science
4921:10.1051/0004-6361/202038935
4842:Planetary and Space Science
4796:Planetary and Space Science
4750:Planetary and Space Science
4277:Planetary and Space Science
4185:Planetary and Space Science
3881:Planetary and Space Science
2645:Planetary and Space Science
2523:Planetary and Space Science
2412:Planetary and Space Science
2254:"The Galileo Dust Detector"
1814:10.1007/978-3-642-56428-4_1
1698:Planetary and Space Science
1512:Helios Dust Instrumentation
1495:
1398:calcium-aluminum inclusions
1122:, a 0.09 m highly-reliable
747:. After its Jupiter flyby,
646:Impact ionization detectors
510:Modern microphone detectors
200:linear particle accelerator
182:in Heidelberg), and at the
61:
10:
7593:
7146:10.1038/s41550-021-01550-6
6831:Stratospheric Dust Samples
6595:Interstellar Dust Explorer
6331:Institute of Space Systems
6216:10.1016/j.nima.2004.07.121
6192:"Large area mass analyzer"
4978:10.1051/0004-6361:20053909
4958:Astronomy and Astrophysics
3800:10.1007/s11214-020-00775-7
3635:Astronomy and Astrophysics
3608:10.1088/0022-3735/20/6/033
2840:Astronomy and Astrophysics
2022:Journal of Applied Physics
1470:magnetic mass spectrometer
1449:space probe orbited comet
1041:mission. In January 2004,
791:Dust composition analyzers
630:During the flyby of comet
6893:Brownlee, D. (May 2014).
6569:10.1016/j.pss.2019.04.005
6333:. University of Stuttgart
6288:10.1109/AERO.2011.5747300
6280:2011 Aerospace Conference
6054:10.1007/s11038-005-9040-z
5715:10.1016/j.pss.2006.05.021
5668:10.1016/j.pss.2006.05.012
5429:10.1007/s11214-004-1435-z
4501:10.1007/s11214-014-0118-7
4251:10.1088/0022-3735/6/3/008
4071:(9): article id. e29645.
3901:10.1016/j.pss.2006.05.021
3028:The Astrophysical Journal
2892:10.1007/3-540-07615-8_448
1802:"Historical Perspectives"
1451:67P/Churyumov–Gerasimenko
317:Zodiacal light photometer
6421:"Europa Clipper Mission"
6034:Earth, Moon, and Planets
5217:(6115): 755–760 (1987).
5160:(6166): 691–695 (1988).
1898:(1): article id.011319.
1392:grains, a wide range of
210:Reliable dust detections
7567:Extragalactic astronomy
7475:2021A&A...645A..38P
7404:2019A&A...630A..32H
7343:2019A&A...630A..26M
7320:Levasseur-Regourd, A.C.
7006:2014M&PS...49.1720W
6957:2012M&PS...47..453B
6561:2019P&SS..172...22K
6507:. University Stuttgart.
6046:2004EM&P...95..211S
5936:10.1126/science.aac6397
5811:10.1126/science.1121375
5707:2006P&SS...54..967S
5660:2006P&SS...54..999K
5366:10.1126/science.1098836
4970:2006A&A...448..243A
4913:2020A&A...643A..96K
4854:1980P&SS...28..333G
4808:1980P&SS...28..321P
4762:1977P&SS...25..135D
4289:1979P&SS...27..511F
4197:1975P&SS...23..183Z
4039:10.1029/GL013i003p00291
3947:10.1029/JA092iA13p14959
3893:2006P&SS...54..967S
3647:1987A&A...187..719M
3323:10.1029/JA085iA11p05841
2852:1978A&A....63..183L
2657:1975P&SS...23..151H
2535:1975P&SS...23..215H
2424:1977P&SS...25..135D
2224:1970E&PSL...8...31N
1892:Applied Physics Reviews
1710:1963P&SS...11.1015E
1463:atomic force microscope
1314:giant-impact hypothesis
1280:Collected dust analyses
1262:University of Stuttgart
1214:University of Stuttgart
1128:polyvinylidene fluoride
1103:(CDA) was flown on the
559:lead zirconate titanate
488:). For example, on the
382:Spitzer Space Telescope
16:Space dust measurements
7297:10.1093/mnras/stab1028
7249:10.1093/mnras/staa2950
6827:"Curation/Cosmic Dust"
6756:10.1073/pnas.36.12.687
4340:10.1006/icar.1997.5789
3748:"Mercury Dust Monitor"
3440:(3): 034501–034501–8.
2143:(7): 075108–075108–8.
1360:
1350:chondritic composition
1181:
1120:chemical dust analyzer
1032:
923:
895:
833:in Heidelberg and the
764:
574:
421:In 1972 and 1973, the
405:
309:
259:
148:
140:
32:Space dust measurement
28:
6487:DESTINY+ Dust Analyze
5409:Space Science Reviews
4667:10.1093/mnras/stx3007
4481:Space Science Reviews
3780:Space Science Reviews
2258:Space Science Reviews
1644:Space Science Reviews
1517:Surface Dust Analyser
1421:encountered asteroid
1358:
1221:Surface Dust Analyser
1178:
1025:
924:
922:{\displaystyle \rho }
896:
837:in Moffet Field. The
762:
579:Plasma Wave Subsystem
572:
565:Chance dust detectors
441:were launched by the
403:
396:Penetration detectors
390:European Space Agency
307:
257:
146:
138:
22:
7075:. pp. 397–418.
6879:10.1029/2003JE002109
6375:10.5194/epsc2021-659
5530:10.1029/2003JA009874
5286:10.1029/2003JE002091
4618:10.1002/2016GL069148
4095:10.1029/2021JA029645
3752:ESA Science Missions
3726:ESA Science Missions
2089:(9): 95111-95111-8.
1989:Procedia Engineering
1850:. Berlin: Springer.
1694:"The zodiacal light"
1502:Cosmic Dust Analyzer
1223:(SUDA) on board the
1194:Cosmic Dust Analyzer
1101:Cosmic Dust Analyzer
913:
845:
835:Ames Research Center
632:21P/Giacobini–Zinner
609:Cosmic Dust Analyzer
540:26P/Grigg–Skjellerup
514:During its flyby of
486:Cosmic Dust Analyzer
250:Microcrater analyses
196:Ames Research Center
165:Johnson Space Center
7520:2014EGUGA..1612830S
7514:. id.12830: 12830.
7288:2021MNRAS.504.4940P
7137:2022NatAs...6..214Y
7081:2015aste.book..397Y
6911:2014AREPS..42..179B
6870:2003JGRE..108.8113T
6806:1977LPSC....8..149B
6747:1950PNAS...36..687W
6666:2001Natur.412..708C
6636:2021AGUFMSH25C2108S
6366:2021EPSC...15..659S
6254:2007ESASP.643..209S
6208:2004NIMPA.535..162R
6154:2011RScI...82j5104X
6100:2008RScI...79h4501A
5990:2000DPS....32.2616G
5928:2016Sci...352..312A
5873:10.1038/nature10175
5865:2011Natur.474..620P
5803:2006Sci...311.1416S
5797:(5766): 1416–1418.
5753:2007MNRAS.377.1588H
5611:2004Icar..171..317K
5562:2006Icar..183..122P
5521:2003JGRA..108.8032A
5475:2007Icar..190..643H
5421:2004SSRv..114..465S
5358:2004Sci...304.1774K
5352:(5678): 1774–1776.
5320:2011epsc.conf.1338K
5278:2003JGRE..108.8114K
5223:1987Natur.326..755K
5166:1988Natur.332..691J
5109:1986Natur.321..280K
5052:1986Natur.321..336K
5020:1986ESASP1070...67K
4724:1975RF.....19..268G
4658:2018MNRAS.474.4225S
4609:2016GeoRL..43.4893S
4555:10.1038/nature14479
4547:2015Natur.522..324H
4493:2014SSRv..185...93H
4439:2003Icar..164..170K
4375:1993Natur.362..428G
4332:1997Icar..129..270G
4243:1973JPhE....6..209D
4141:1969RScI...40.1333B
4087:2021JGRA..12629645S
4031:1986GeoRL..13..291G
3985:1991JGR....9619177G
3939:1987JGR....9214959G
3846:1983Icar...53..236G
3792:2020SSRv..216..144K
3685:1993Natur.362..732M
3600:1987JPhE...20..741M
3546:2019Icar..321..116P
3500:2008Icar..193..420K
3446:2010RScI...81c4501J
3392:1986Natur.321..278S
3315:1980JGR....85.5841H
3277:1966NASTN3717.....N
3175:2007Icar..191..298R
3123:1992Icar...95..180S
3050:1998ApJ...508...44K
2981:1974Sci...186..650A
2940:1971NASSP.267..617S
2884:1976LNP....48...29H
2814:1992LPSC...22..185M
2752:1993Sci...262..550L
2706:1985Icar...62..244G
2619:1979LPSC...10.1649M
2581:1977LPSC....8..841M
2497:1973spre.conf.1057G
2485:Space Research XIII
2370:1978RScI...49....1V
2316:2017RScI...88c4501T
2270:1992SSRv...60..317G
2149:2012RScI...83g5108S
2095:2011RScI...82i5111M
2034:1960JAP....31.1243S
1914:2021ApPRv...8a1319V
1856:2001indu.book.....G
1847:Interplanetary Dust
1806:Interplanetary Dust
1756:1966Sci...153.1242N
1750:(3741): 1242–1246.
1656:1968SSRv....8..455N
1618:1963SCoA....7...71M
1564:1961Natur.192..441M
1296:aspects—from their
1136:interplanetary dust
871:
859:
685:interplanetary dust
661:has been explored.
348:interplanetary dust
204:quadrupole ion trap
125:Interplanetary Dust
72:scattered sun light
7572:Galactic astronomy
7199:Curation/Hayabusa2
7015:10.1111/maps.12221
6630:. id. SH25C-2108.
5654:(9–10): 999–1006.
5103:: 280–282 (1986).
5046:: 336–337 (1986).
4712:Raumfahrtforschung
2278:10.1007/BF00216860
1664:10.1007/BF00184742
1361:
1284:The importance of
1182:
1162:'s close flyby of
1158:. In 2005, during
1067:mass spectrometers
1033:
1001:mass spectrometers
919:
891:
881:
866:
823:mass spectrometers
781:microchannel plate
765:
675:space probes. The
575:
439:Pegasus satellites
406:
369:(DIRBE) on NASA's
359:infrared astronomy
310:
260:
149:
141:
29:
7577:Planetary science
7547:Space exploration
7173:Curation/Hayabusa
6660:(6848): 708–712.
6297:978-1-4244-7350-2
6162:10.1063/1.3646528
6108:10.1063/1.2960566
6007:978-0-08-044194-8
5922:(6283): 312–318.
5859:(7353): 620–622.
5701:(9–10): 967–987.
4603:(10): 4893–4898.
4541:(7556): 324–326.
4369:(6419): 428–430.
4149:10.1063/1.1683778
4135:(10): 1333–1337.
3993:10.1029/91JA01270
3454:10.1063/1.3340880
2975:(4164): 650–652.
2901:978-3-540-07615-5
2746:(5133): 550–553.
2378:10.1063/1.1135244
2324:10.1063/1.4977832
2157:10.1063/1.4732820
2103:10.1063/1.3637461
2042:10.1063/1.1735813
1923:10.1063/5.0040772
1865:978-3-540-42067-5
1823:978-3-642-62647-0
1558:(4801): 441–442.
1140:interstellar dust
1124:impact ionization
1064:impact ionization
987:impact ionization
942:interstellar dust
883:
870:
858:
817:impact ionization
737:swing-by maneuver
651:Impact ionization
240:impact ionization
191:impact ionization
157:muzzle velocities
131:Dust accelerators
113:, and the Soviet
82:. By observing a
66:From the ground,
7584:
7531:
7530:
7528:
7526:
7509:
7500:
7494:
7493:
7491:
7489:
7468:
7450:
7437:
7431:
7430:
7428:
7426:
7389:
7376:
7370:
7369:
7367:
7365:
7328:
7315:
7309:
7308:
7306:
7304:
7299:
7282:(4): 4940–4951.
7267:
7261:
7260:
7258:
7256:
7251:
7241:
7232:(2): 1870–1873.
7217:
7211:
7210:
7208:
7206:
7191:
7185:
7184:
7182:
7180:
7165:
7159:
7158:
7148:
7125:Nature Astronomy
7116:
7110:
7109:
7107:
7105:
7060:
7054:
7053:
7051:
7049:
7034:
7028:
7027:
7017:
7000:(9): 1720–1733.
6985:
6979:
6978:
6968:
6936:
6930:
6929:
6927:
6925:
6890:
6884:
6883:
6881:
6849:
6843:
6842:
6840:
6838:
6823:
6817:
6816:
6814:
6812:
6785:
6779:
6778:
6768:
6758:
6726:
6720:
6719:
6717:
6715:
6700:
6694:
6693:
6674:10.1038/35089010
6646:
6640:
6639:
6623:
6617:
6616:
6605:
6599:
6598:
6587:
6581:
6580:
6554:
6533:
6527:
6526:
6515:
6509:
6508:
6497:
6491:
6490:
6479:
6473:
6472:
6461:
6455:
6454:
6443:
6437:
6436:
6434:
6432:
6417:
6411:
6401:
6395:
6394:
6392:
6390:
6377:
6349:
6343:
6342:
6340:
6338:
6323:
6317:
6316:
6314:
6312:
6282:. pp. 1–8.
6271:
6265:
6264:
6262:
6260:
6233:
6227:
6226:
6224:
6222:
6202:(1–2): 162–164.
6187:
6181:
6180:
6178:
6176:
6133:
6127:
6126:
6124:
6122:
6079:
6073:
6072:
6070:
6068:
6040:(1–4): 211–220.
6025:
6019:
6018:
6016:
6014:
5969:
5963:
5962:
5960:
5958:
5906:
5900:
5899:
5897:
5895:
5844:
5838:
5837:
5835:
5833:
5781:
5775:
5774:
5764:
5747:(4): 1588–1596.
5732:
5726:
5725:
5723:
5721:
5685:
5679:
5678:
5676:
5674:
5639:
5630:
5629:
5627:
5625:
5590:
5581:
5580:
5578:
5576:
5541:
5535:
5534:
5532:
5500:
5494:
5493:
5491:
5489:
5454:
5448:
5447:
5445:
5443:
5415:(1–4): 465–518.
5399:
5393:
5392:
5390:
5388:
5337:
5331:
5330:
5328:
5326:
5305:
5296:
5290:
5289:
5256:
5250:
5249:
5247:
5245:
5231:10.1038/326755a0
5208:
5199:
5193:
5192:
5190:
5188:
5174:10.1038/332691a0
5151:
5142:
5136:
5135:
5133:
5131:
5117:10.1038/321280a0
5094:
5085:
5079:
5078:
5076:
5074:
5060:10.1038/321336a0
5030:
5024:
5023:
5003:
4997:
4996:
4994:
4992:
4955:
4946:
4940:
4939:
4937:
4935:
4906:
4888:
4879:
4873:
4872:
4870:
4868:
4833:
4827:
4826:
4824:
4822:
4787:
4781:
4780:
4778:
4776:
4741:
4735:
4734:
4732:
4730:
4703:
4697:
4696:
4694:
4692:
4679:
4669:
4652:(3): 4225–4231.
4637:
4631:
4630:
4620:
4588:
4582:
4581:
4579:
4577:
4526:
4520:
4519:
4517:
4515:
4472:
4466:
4465:
4463:
4461:
4432:
4430:astro-ph/0304381
4408:
4402:
4401:
4399:
4397:
4383:10.1038/362428a0
4353:
4344:
4343:
4314:
4308:
4307:
4305:
4303:
4268:
4262:
4261:
4259:
4257:
4222:
4216:
4215:
4213:
4211:
4176:
4170:
4169:
4167:
4165:
4160:
4158:2060/19690021680
4120:
4114:
4113:
4111:
4109:
4080:
4056:
4050:
4049:
4047:
4045:
4010:
4004:
4003:
4001:
3999:
3964:
3958:
3957:
3955:
3953:
3918:
3912:
3911:
3909:
3907:
3871:
3865:
3864:
3862:
3860:
3825:
3819:
3818:
3816:
3814:
3770:
3764:
3763:
3761:
3759:
3744:
3738:
3737:
3735:
3733:
3718:
3712:
3711:
3709:
3707:
3693:10.1038/362732a0
3664:
3658:
3657:
3655:
3653:
3625:
3619:
3618:
3616:
3614:
3579:
3573:
3572:
3570:
3568:
3525:
3519:
3518:
3516:
3514:
3479:
3473:
3472:
3470:
3468:
3425:
3419:
3418:
3416:
3414:
3400:10.1038/321278a0
3370:
3364:
3363:
3361:
3359:
3349:
3340:
3334:
3333:
3331:
3329:
3294:
3288:
3287:
3285:
3283:
3256:
3247:
3246:
3244:
3242:
3227:
3221:
3220:
3218:
3216:
3210:
3201:
3195:
3194:
3168:
3148:
3142:
3141:
3139:
3137:
3102:
3096:
3095:
3093:
3091:
3076:
3070:
3069:
3043:
3041:astro-ph/9806250
3022:
3016:
3015:
3013:
3011:
2960:
2951:
2950:
2948:
2946:
2919:
2913:
2912:
2910:
2908:
2869:
2863:
2862:
2860:
2858:
2831:
2825:
2824:
2822:
2820:
2793:
2787:
2786:
2784:
2782:
2731:
2725:
2724:
2722:
2720:
2685:
2676:
2675:
2673:
2671:
2636:
2630:
2629:
2627:
2625:
2598:
2592:
2591:
2589:
2587:
2560:
2554:
2553:
2551:
2549:
2514:
2508:
2507:
2505:
2503:
2476:
2470:
2469:
2467:
2465:
2449:
2443:
2442:
2440:
2438:
2403:
2397:
2396:
2394:
2392:
2349:
2343:
2342:
2340:
2338:
2310:(3): id.034501.
2295:
2289:
2288:
2286:
2284:
2264:(1–4): 317–340.
2249:
2243:
2242:
2240:
2238:
2203:
2197:
2196:
2194:
2192:
2182:
2176:
2175:
2173:
2171:
2128:
2122:
2121:
2119:
2117:
2073:
2067:
2066:
2059:
2053:
2052:
2050:
2048:
2013:
2007:
2006:
2004:
1980:
1974:
1973:
1971:
1969:
1960:
1952:
1946:
1945:
1935:
1925:
1907:
1883:
1877:
1876:
1874:
1872:
1841:
1835:
1834:
1832:
1830:
1797:
1791:
1790:
1788:
1786:
1735:
1729:
1728:
1726:
1724:
1704:(9): 1015–1033.
1689:
1683:
1682:
1680:
1678:
1635:
1629:
1628:
1626:
1624:
1597:
1591:
1590:
1588:
1586:
1572:10.1038/192441b0
1543:
1138:, the stream of
928:
926:
925:
920:
900:
898:
897:
892:
884:
882:
880:
867:
865:
855:
163:(e.g. at NASA's
40:carbon compounds
7592:
7591:
7587:
7586:
7585:
7583:
7582:
7581:
7537:
7536:
7535:
7534:
7524:
7522:
7507:
7501:
7497:
7487:
7485:
7448:
7438:
7434:
7424:
7422:
7387:
7377:
7373:
7363:
7361:
7326:
7316:
7312:
7302:
7300:
7268:
7264:
7254:
7252:
7218:
7214:
7204:
7202:
7193:
7192:
7188:
7178:
7176:
7167:
7166:
7162:
7117:
7113:
7103:
7101:
7099:
7061:
7057:
7047:
7045:
7036:
7035:
7031:
6986:
6982:
6937:
6933:
6923:
6921:
6891:
6887:
6850:
6846:
6836:
6834:
6825:
6824:
6820:
6810:
6808:
6786:
6782:
6741:(12): 687–695.
6727:
6723:
6713:
6711:
6702:
6701:
6697:
6647:
6643:
6624:
6620:
6607:
6606:
6602:
6589:
6588:
6584:
6534:
6530:
6517:
6516:
6512:
6499:
6498:
6494:
6481:
6480:
6476:
6463:
6462:
6458:
6445:
6444:
6440:
6430:
6428:
6419:
6418:
6414:
6402:
6398:
6388:
6386:
6350:
6346:
6336:
6334:
6325:
6324:
6320:
6310:
6308:
6298:
6272:
6268:
6258:
6256:
6234:
6230:
6220:
6218:
6188:
6184:
6174:
6172:
6134:
6130:
6120:
6118:
6080:
6076:
6066:
6064:
6026:
6022:
6012:
6010:
6008:
5970:
5966:
5956:
5954:
5907:
5903:
5893:
5891:
5845:
5841:
5831:
5829:
5782:
5778:
5733:
5729:
5719:
5717:
5686:
5682:
5672:
5670:
5640:
5633:
5623:
5621:
5591:
5584:
5574:
5572:
5542:
5538:
5501:
5497:
5487:
5485:
5455:
5451:
5441:
5439:
5400:
5396:
5386:
5384:
5338:
5334:
5324:
5322:
5303:
5297:
5293:
5257:
5253:
5243:
5241:
5206:
5200:
5196:
5186:
5184:
5149:
5143:
5139:
5129:
5127:
5092:
5086:
5082:
5072:
5070:
5031:
5027:
5004:
5000:
4990:
4988:
4953:
4947:
4943:
4933:
4931:
4897:(id. A96): 13.
4886:
4880:
4876:
4866:
4864:
4834:
4830:
4820:
4818:
4788:
4784:
4774:
4772:
4742:
4738:
4728:
4726:
4704:
4700:
4690:
4688:
4638:
4634:
4589:
4585:
4575:
4573:
4527:
4523:
4513:
4511:
4473:
4469:
4459:
4457:
4409:
4405:
4395:
4393:
4354:
4347:
4315:
4311:
4301:
4299:
4269:
4265:
4255:
4253:
4223:
4219:
4209:
4207:
4177:
4173:
4163:
4161:
4121:
4117:
4107:
4105:
4057:
4053:
4043:
4041:
4011:
4007:
3997:
3995:
3965:
3961:
3951:
3949:
3919:
3915:
3905:
3903:
3872:
3868:
3858:
3856:
3826:
3822:
3812:
3810:
3771:
3767:
3757:
3755:
3746:
3745:
3741:
3731:
3729:
3720:
3719:
3715:
3705:
3703:
3665:
3661:
3651:
3649:
3626:
3622:
3612:
3610:
3580:
3576:
3566:
3564:
3526:
3522:
3512:
3510:
3480:
3476:
3466:
3464:
3426:
3422:
3412:
3410:
3371:
3367:
3357:
3355:
3347:
3341:
3337:
3327:
3325:
3295:
3291:
3281:
3279:
3257:
3250:
3240:
3238:
3229:
3228:
3224:
3214:
3212:
3208:
3202:
3198:
3149:
3145:
3135:
3133:
3103:
3099:
3089:
3087:
3078:
3077:
3073:
3023:
3019:
3009:
3007:
2961:
2954:
2944:
2942:
2920:
2916:
2906:
2904:
2902:
2870:
2866:
2856:
2854:
2832:
2828:
2818:
2816:
2794:
2790:
2780:
2778:
2732:
2728:
2718:
2716:
2686:
2679:
2669:
2667:
2637:
2633:
2623:
2621:
2599:
2595:
2585:
2583:
2561:
2557:
2547:
2545:
2515:
2511:
2501:
2499:
2477:
2473:
2463:
2461:
2450:
2446:
2436:
2434:
2404:
2400:
2390:
2388:
2350:
2346:
2336:
2334:
2296:
2292:
2282:
2280:
2250:
2246:
2236:
2234:
2204:
2200:
2190:
2188:
2184:
2183:
2179:
2169:
2167:
2129:
2125:
2115:
2113:
2074:
2070:
2061:
2060:
2056:
2046:
2044:
2014:
2010:
1981:
1977:
1967:
1965:
1958:
1954:
1953:
1949:
1884:
1880:
1870:
1868:
1866:
1842:
1838:
1828:
1826:
1824:
1798:
1794:
1784:
1782:
1736:
1732:
1722:
1720:
1690:
1686:
1676:
1674:
1636:
1632:
1622:
1620:
1598:
1594:
1584:
1582:
1544:
1540:
1535:
1498:
1472:(DFMS) and the
1438:C-type asteroid
1390:silicon carbide
1386:presolar grains
1330:Luna spacecraft
1318:Apollo missions
1282:
1173:
1171:Dust Telescopes
1156:Saturn's E ring
1134:, CDA analyzed
995:reflectron type
939:
934:
914:
911:
910:
873:
868:
861:
856:
854:
846:
843:
842:
839:mass resolution
813:micrometeoroids
793:
648:
567:
512:
482:Cassini–Huygens
398:
378:cometary trails
319:instruments on
302:
287:low Earth orbit
252:
212:
133:
70:is observed as
64:
17:
12:
11:
5:
7590:
7580:
7579:
7574:
7569:
7564:
7562:Astrochemistry
7559:
7554:
7549:
7533:
7532:
7495:
7432:
7371:
7310:
7262:
7212:
7186:
7160:
7131:(2): 214–220.
7111:
7097:
7055:
7029:
6980:
6951:(4): 453–470.
6931:
6905:(1): 179–205.
6885:
6844:
6818:
6780:
6721:
6708:Curation/Lunar
6695:
6641:
6618:
6600:
6582:
6528:
6510:
6492:
6474:
6456:
6438:
6425:Europa Clipper
6412:
6408:EPSC Abstracts
6396:
6344:
6318:
6296:
6266:
6228:
6182:
6128:
6074:
6020:
6006:
5964:
5901:
5839:
5776:
5727:
5680:
5631:
5605:(2): 317–335.
5582:
5556:(1): 122–134.
5536:
5495:
5469:(2): 643–654.
5449:
5394:
5332:
5291:
5251:
5194:
5137:
5080:
5025:
4998:
4941:
4874:
4848:(3): 333–349.
4828:
4802:(3): 321–331.
4782:
4756:(2): 135–147.
4736:
4698:
4632:
4583:
4521:
4467:
4423:(1): 170–187.
4403:
4345:
4326:(2): 270–288.
4309:
4283:(4): 511–531.
4263:
4237:(3): 209–217.
4217:
4191:(4): 183–203.
4171:
4115:
4051:
4005:
3959:
3933:(A13): 14959.
3913:
3866:
3820:
3765:
3739:
3713:
3659:
3620:
3574:
3520:
3474:
3420:
3365:
3343:Naumann, R.J.
3335:
3289:
3248:
3222:
3196:
3143:
3097:
3071:
3058:10.1086/306380
3017:
2952:
2914:
2900:
2864:
2826:
2788:
2726:
2700:(2): 244–272.
2677:
2631:
2593:
2555:
2529:(1): 215–224.
2509:
2471:
2444:
2398:
2344:
2290:
2244:
2198:
2177:
2123:
2068:
2054:
2008:
1975:
1947:
1878:
1864:
1836:
1822:
1792:
1730:
1684:
1650:(3): 455–466.
1630:
1592:
1537:
1536:
1534:
1531:
1530:
1529:
1524:
1519:
1514:
1509:
1504:
1497:
1494:
1394:chondrule-like
1281:
1278:
1274:Lagrange point
1248:space mission
1235:Europa Clipper
1226:Europa Clipper
1208:(LASP) of the
1186:dust astronomy
1172:
1169:
1053:flew by comet
1045:flew by comet
998:time-of-flight
949:Halley's Comet
937:
932:
918:
890:
887:
879:
876:
864:
853:
850:
820:time-of-flight
792:
789:
785:lunar regolith
745:Galilean moons
714:dust detectors
647:
644:
566:
563:
527:Whipple shield
516:Halley's Comet
511:
508:
397:
394:
313:Zodiacal light
301:
298:
291:Space Shuttle
251:
248:
211:
208:
198:, ARC, used a
161:light-gas guns
132:
129:
63:
60:
50:, optical and
15:
9:
6:
4:
3:
2:
7589:
7578:
7575:
7573:
7570:
7568:
7565:
7563:
7560:
7558:
7555:
7553:
7550:
7548:
7545:
7544:
7542:
7521:
7517:
7513:
7506:
7499:
7484:
7480:
7476:
7472:
7467:
7462:
7458:
7454:
7447:
7443:
7440:Pestoni, B.;
7436:
7421:
7417:
7413:
7409:
7405:
7401:
7397:
7393:
7386:
7382:
7375:
7360:
7356:
7352:
7348:
7344:
7340:
7336:
7332:
7325:
7321:
7314:
7298:
7293:
7289:
7285:
7281:
7277:
7273:
7266:
7250:
7245:
7240:
7235:
7231:
7227:
7223:
7216:
7200:
7196:
7190:
7174:
7170:
7164:
7156:
7152:
7147:
7142:
7138:
7134:
7130:
7126:
7122:
7115:
7100:
7098:9780816532131
7094:
7090:
7086:
7082:
7078:
7074:
7070:
7066:
7059:
7043:
7039:
7033:
7025:
7021:
7016:
7011:
7007:
7003:
6999:
6995:
6991:
6984:
6976:
6972:
6967:
6962:
6958:
6954:
6950:
6946:
6942:
6935:
6920:
6916:
6912:
6908:
6904:
6900:
6896:
6889:
6880:
6875:
6871:
6867:
6864:(E10): 8113.
6863:
6859:
6855:
6848:
6832:
6828:
6822:
6807:
6803:
6799:
6795:
6791:
6784:
6776:
6772:
6767:
6762:
6757:
6752:
6748:
6744:
6740:
6736:
6732:
6725:
6709:
6705:
6699:
6691:
6687:
6683:
6679:
6675:
6671:
6667:
6663:
6659:
6655:
6651:
6645:
6637:
6633:
6629:
6622:
6614:
6610:
6604:
6596:
6592:
6586:
6578:
6574:
6570:
6566:
6562:
6558:
6553:
6548:
6544:
6540:
6532:
6524:
6520:
6514:
6506:
6502:
6496:
6488:
6484:
6478:
6470:
6466:
6460:
6452:
6448:
6442:
6426:
6422:
6416:
6409:
6405:
6400:
6385:
6381:
6376:
6371:
6367:
6363:
6359:
6355:
6348:
6332:
6328:
6322:
6307:
6303:
6299:
6293:
6289:
6285:
6281:
6277:
6270:
6255:
6251:
6247:
6243:
6239:
6232:
6217:
6213:
6209:
6205:
6201:
6197:
6193:
6186:
6171:
6167:
6163:
6159:
6155:
6151:
6147:
6143:
6139:
6132:
6117:
6113:
6109:
6105:
6101:
6097:
6093:
6089:
6085:
6078:
6063:
6059:
6055:
6051:
6047:
6043:
6039:
6035:
6031:
6024:
6009:
6003:
5999:
5995:
5991:
5987:
5983:
5979:
5975:
5968:
5953:
5949:
5945:
5941:
5937:
5933:
5929:
5925:
5921:
5917:
5913:
5905:
5890:
5886:
5882:
5878:
5874:
5870:
5866:
5862:
5858:
5854:
5850:
5843:
5828:
5824:
5820:
5816:
5812:
5808:
5804:
5800:
5796:
5792:
5788:
5780:
5772:
5768:
5763:
5758:
5754:
5750:
5746:
5742:
5738:
5731:
5716:
5712:
5708:
5704:
5700:
5696:
5692:
5684:
5669:
5665:
5661:
5657:
5653:
5649:
5645:
5638:
5636:
5620:
5616:
5612:
5608:
5604:
5600:
5596:
5589:
5587:
5571:
5567:
5563:
5559:
5555:
5551:
5547:
5540:
5531:
5526:
5522:
5518:
5515:(A10): 8032.
5514:
5510:
5506:
5499:
5484:
5480:
5476:
5472:
5468:
5464:
5460:
5453:
5438:
5434:
5430:
5426:
5422:
5418:
5414:
5410:
5406:
5398:
5383:
5379:
5375:
5371:
5367:
5363:
5359:
5355:
5351:
5347:
5343:
5336:
5321:
5317:
5313:
5309:
5302:
5295:
5287:
5283:
5279:
5275:
5272:(E10): 8114.
5271:
5267:
5263:
5255:
5240:
5236:
5232:
5228:
5224:
5220:
5216:
5212:
5205:
5198:
5183:
5179:
5175:
5171:
5167:
5163:
5159:
5155:
5148:
5141:
5126:
5122:
5118:
5114:
5110:
5106:
5102:
5098:
5091:
5084:
5069:
5065:
5061:
5057:
5053:
5049:
5045:
5041:
5037:
5029:
5021:
5017:
5013:
5009:
5002:
4987:
4983:
4979:
4975:
4971:
4967:
4963:
4959:
4952:
4945:
4930:
4926:
4922:
4918:
4914:
4910:
4905:
4900:
4896:
4892:
4885:
4878:
4863:
4859:
4855:
4851:
4847:
4843:
4839:
4832:
4817:
4813:
4809:
4805:
4801:
4797:
4793:
4786:
4771:
4767:
4763:
4759:
4755:
4751:
4747:
4740:
4725:
4721:
4717:
4713:
4709:
4702:
4687:
4683:
4678:
4673:
4668:
4663:
4659:
4655:
4651:
4647:
4643:
4636:
4628:
4624:
4619:
4614:
4610:
4606:
4602:
4598:
4594:
4587:
4572:
4568:
4564:
4560:
4556:
4552:
4548:
4544:
4540:
4536:
4532:
4525:
4510:
4506:
4502:
4498:
4494:
4490:
4486:
4482:
4478:
4471:
4456:
4452:
4448:
4444:
4440:
4436:
4431:
4426:
4422:
4418:
4414:
4407:
4392:
4388:
4384:
4380:
4376:
4372:
4368:
4364:
4360:
4352:
4350:
4341:
4337:
4333:
4329:
4325:
4321:
4313:
4298:
4294:
4290:
4286:
4282:
4278:
4274:
4267:
4252:
4248:
4244:
4240:
4236:
4232:
4228:
4221:
4206:
4202:
4198:
4194:
4190:
4186:
4182:
4175:
4159:
4154:
4150:
4146:
4142:
4138:
4134:
4130:
4126:
4119:
4104:
4100:
4096:
4092:
4088:
4084:
4079:
4074:
4070:
4066:
4062:
4055:
4040:
4036:
4032:
4028:
4024:
4020:
4016:
4009:
3994:
3990:
3986:
3982:
3978:
3974:
3970:
3963:
3948:
3944:
3940:
3936:
3932:
3928:
3924:
3917:
3902:
3898:
3894:
3890:
3886:
3882:
3878:
3870:
3855:
3851:
3847:
3843:
3839:
3835:
3831:
3824:
3809:
3805:
3801:
3797:
3793:
3789:
3785:
3781:
3777:
3769:
3753:
3749:
3743:
3727:
3723:
3717:
3702:
3698:
3694:
3690:
3686:
3682:
3679:(6422): 732.
3678:
3674:
3670:
3663:
3648:
3644:
3640:
3636:
3632:
3624:
3609:
3605:
3601:
3597:
3593:
3589:
3585:
3578:
3563:
3559:
3555:
3551:
3547:
3543:
3539:
3535:
3531:
3524:
3509:
3505:
3501:
3497:
3493:
3489:
3485:
3478:
3463:
3459:
3455:
3451:
3447:
3443:
3439:
3435:
3431:
3424:
3409:
3405:
3401:
3397:
3393:
3389:
3385:
3381:
3377:
3369:
3353:
3346:
3339:
3324:
3320:
3316:
3312:
3309:(A11): 5841.
3308:
3304:
3300:
3293:
3278:
3274:
3270:
3266:
3262:
3255:
3253:
3236:
3232:
3226:
3207:
3200:
3192:
3188:
3184:
3180:
3176:
3172:
3167:
3162:
3158:
3154:
3147:
3132:
3128:
3124:
3120:
3116:
3112:
3108:
3101:
3085:
3081:
3080:"COBE Images"
3075:
3067:
3063:
3059:
3055:
3051:
3047:
3042:
3037:
3033:
3029:
3021:
3006:
3002:
2998:
2994:
2990:
2986:
2982:
2978:
2974:
2970:
2966:
2959:
2957:
2941:
2937:
2933:
2929:
2925:
2918:
2903:
2897:
2893:
2889:
2885:
2881:
2877:
2876:
2868:
2853:
2849:
2845:
2841:
2837:
2830:
2815:
2811:
2807:
2803:
2799:
2792:
2777:
2773:
2769:
2765:
2761:
2757:
2753:
2749:
2745:
2741:
2737:
2730:
2715:
2711:
2707:
2703:
2699:
2695:
2691:
2684:
2682:
2666:
2662:
2658:
2654:
2650:
2646:
2642:
2635:
2620:
2616:
2612:
2608:
2604:
2597:
2582:
2578:
2574:
2570:
2566:
2559:
2544:
2540:
2536:
2532:
2528:
2524:
2520:
2513:
2498:
2494:
2491:: 1057–1062.
2490:
2486:
2482:
2475:
2459:
2455:
2448:
2433:
2429:
2425:
2421:
2417:
2413:
2409:
2402:
2387:
2383:
2379:
2375:
2371:
2367:
2363:
2359:
2355:
2348:
2333:
2329:
2325:
2321:
2317:
2313:
2309:
2305:
2301:
2294:
2279:
2275:
2271:
2267:
2263:
2259:
2255:
2248:
2233:
2229:
2225:
2221:
2217:
2213:
2209:
2202:
2187:
2181:
2166:
2162:
2158:
2154:
2150:
2146:
2142:
2138:
2134:
2127:
2112:
2108:
2104:
2100:
2096:
2092:
2088:
2084:
2080:
2072:
2064:
2058:
2043:
2039:
2035:
2031:
2027:
2023:
2019:
2012:
2003:
1998:
1994:
1990:
1986:
1979:
1964:
1957:
1951:
1943:
1939:
1934:
1933:1721.1/141164
1929:
1924:
1919:
1915:
1911:
1906:
1901:
1897:
1893:
1889:
1882:
1867:
1861:
1857:
1853:
1849:
1848:
1840:
1825:
1819:
1815:
1811:
1807:
1803:
1796:
1781:
1777:
1773:
1769:
1765:
1761:
1757:
1753:
1749:
1745:
1741:
1734:
1719:
1715:
1711:
1707:
1703:
1699:
1695:
1688:
1673:
1669:
1665:
1661:
1657:
1653:
1649:
1645:
1641:
1634:
1619:
1615:
1611:
1607:
1603:
1596:
1581:
1577:
1573:
1569:
1565:
1561:
1557:
1553:
1549:
1542:
1538:
1528:
1525:
1523:
1520:
1518:
1515:
1513:
1510:
1508:
1505:
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1486:Philae lander
1483:
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1456:
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1423:25143 Itokawa
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1311:
1310:mineralogical
1307:
1303:
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1294:cosmochemical
1291:
1287:
1286:lunar samples
1277:
1275:
1271:
1266:
1263:
1259:
1255:
1254:3200 Phaethon
1251:
1247:
1243:
1238:
1236:
1232:
1228:
1227:
1222:
1217:
1215:
1211:
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1148:magnetosphere
1145:
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1125:
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1109:
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1102:
1097:
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1079:
1074:
1073:
1069:flown on the
1068:
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1039:
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1020:
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904:
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848:
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836:
832:
828:
827:parylene film
824:
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669:
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628:
626:
622:
619:'s flybys of
618:
614:
610:
607:
606:
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595:
592:
591:
586:
585:
581:(PWS) on the
580:
571:
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541:
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454:In 1986, the
452:
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419:
418:
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393:
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244:magnetosphere
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88:triangulation
85:
81:
78:entering the
77:
73:
69:
59:
57:
53:
49:
45:
41:
37:
33:
26:
21:
7557:Astrobiology
7523:. Retrieved
7511:
7498:
7486:. Retrieved
7459:(A36): A38.
7456:
7452:
7435:
7423:. Retrieved
7395:
7391:
7374:
7362:. Retrieved
7334:
7330:
7313:
7301:. Retrieved
7279:
7275:
7265:
7253:. Retrieved
7229:
7225:
7215:
7203:. Retrieved
7198:
7189:
7177:. Retrieved
7172:
7163:
7128:
7124:
7114:
7102:. Retrieved
7069:Asteroids IV
7068:
7058:
7046:. Retrieved
7041:
7032:
6997:
6993:
6983:
6948:
6944:
6934:
6922:. Retrieved
6902:
6898:
6888:
6861:
6857:
6847:
6835:. Retrieved
6830:
6821:
6809:. Retrieved
6797:
6793:
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6738:
6734:
6724:
6712:. Retrieved
6707:
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6504:
6495:
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6477:
6468:
6459:
6450:
6441:
6429:. Retrieved
6424:
6415:
6407:
6399:
6387:. Retrieved
6357:
6347:
6335:. Retrieved
6330:
6321:
6309:. Retrieved
6279:
6269:
6257:. Retrieved
6245:
6241:
6231:
6219:. Retrieved
6199:
6195:
6185:
6173:. Retrieved
6145:
6141:
6131:
6119:. Retrieved
6091:
6087:
6077:
6065:. Retrieved
6037:
6033:
6023:
6011:. Retrieved
5981:
5977:
5967:
5955:. Retrieved
5919:
5915:
5904:
5892:. Retrieved
5856:
5852:
5842:
5830:. Retrieved
5794:
5790:
5779:
5744:
5740:
5730:
5718:. Retrieved
5698:
5694:
5683:
5671:. Retrieved
5651:
5647:
5622:. Retrieved
5602:
5598:
5573:. Retrieved
5553:
5549:
5539:
5512:
5508:
5498:
5486:. Retrieved
5466:
5462:
5452:
5440:. Retrieved
5412:
5408:
5397:
5385:. Retrieved
5349:
5345:
5335:
5323:. Retrieved
5311:
5307:
5294:
5269:
5265:
5254:
5242:. Retrieved
5214:
5210:
5197:
5185:. Retrieved
5157:
5153:
5140:
5128:. Retrieved
5100:
5096:
5083:
5071:. Retrieved
5043:
5039:
5028:
5011:
5007:
5001:
4989:. Retrieved
4961:
4957:
4944:
4932:. Retrieved
4894:
4890:
4877:
4865:. Retrieved
4845:
4841:
4831:
4819:. Retrieved
4799:
4795:
4785:
4773:. Retrieved
4753:
4749:
4739:
4727:. Retrieved
4715:
4711:
4701:
4689:. Retrieved
4649:
4645:
4635:
4600:
4596:
4586:
4574:. Retrieved
4538:
4534:
4524:
4512:. Retrieved
4484:
4480:
4470:
4458:. Retrieved
4420:
4416:
4406:
4394:. Retrieved
4366:
4362:
4323:
4319:
4312:
4300:. Retrieved
4280:
4276:
4266:
4254:. Retrieved
4234:
4230:
4220:
4208:. Retrieved
4188:
4184:
4174:
4162:. Retrieved
4132:
4128:
4118:
4106:. Retrieved
4068:
4064:
4054:
4042:. Retrieved
4022:
4018:
4008:
3996:. Retrieved
3976:
3972:
3962:
3950:. Retrieved
3930:
3926:
3916:
3904:. Retrieved
3884:
3880:
3869:
3857:. Retrieved
3837:
3833:
3823:
3811:. Retrieved
3783:
3779:
3768:
3756:. Retrieved
3751:
3742:
3730:. Retrieved
3725:
3716:
3704:. Retrieved
3676:
3672:
3662:
3650:. Retrieved
3638:
3634:
3623:
3611:. Retrieved
3591:
3587:
3577:
3565:. Retrieved
3537:
3533:
3523:
3511:. Retrieved
3491:
3487:
3477:
3465:. Retrieved
3437:
3433:
3423:
3411:. Retrieved
3383:
3379:
3368:
3356:. Retrieved
3351:
3338:
3326:. Retrieved
3306:
3302:
3292:
3280:. Retrieved
3268:
3264:
3239:. Retrieved
3234:
3225:
3213:. Retrieved
3199:
3156:
3152:
3146:
3134:. Retrieved
3114:
3110:
3100:
3088:. Retrieved
3083:
3074:
3034:(1): 44–73.
3031:
3027:
3020:
3008:. Retrieved
2972:
2968:
2943:. Retrieved
2931:
2927:
2917:
2905:. Retrieved
2874:
2867:
2855:. Retrieved
2846:(1–2): 183.
2843:
2839:
2829:
2817:. Retrieved
2805:
2801:
2791:
2779:. Retrieved
2743:
2739:
2729:
2717:. Retrieved
2697:
2693:
2668:. Retrieved
2648:
2644:
2634:
2622:. Retrieved
2610:
2606:
2596:
2584:. Retrieved
2572:
2568:
2558:
2546:. Retrieved
2526:
2522:
2512:
2500:. Retrieved
2488:
2484:
2474:
2462:. Retrieved
2457:
2447:
2435:. Retrieved
2415:
2411:
2401:
2389:. Retrieved
2361:
2357:
2347:
2335:. Retrieved
2307:
2303:
2293:
2281:. Retrieved
2261:
2257:
2247:
2235:. Retrieved
2215:
2211:
2201:
2189:. Retrieved
2180:
2168:. Retrieved
2140:
2136:
2126:
2114:. Retrieved
2086:
2082:
2071:
2057:
2045:. Retrieved
2025:
2021:
2011:
1992:
1988:
1978:
1966:. Retrieved
1962:
1950:
1895:
1891:
1881:
1869:. Retrieved
1846:
1839:
1827:. Retrieved
1805:
1795:
1783:. Retrieved
1747:
1743:
1733:
1721:. Retrieved
1701:
1697:
1687:
1675:. Retrieved
1647:
1643:
1633:
1621:. Retrieved
1609:
1605:
1595:
1583:. Retrieved
1555:
1551:
1541:
1488:carried the
1481:
1454:
1444:
1442:
1434:162173 Ryugu
1427:
1418:
1412:
1403:
1388:like C-rich
1381:
1374:Comet Wild 2
1369:
1363:
1362:
1346:Don Brownlee
1341:Fred Whipple
1338:
1283:
1267:
1252:to asteroid
1239:
1234:
1224:
1218:
1197:
1189:
1183:
1159:
1151:
1115:
1105:
1098:
1089:
1082:
1076:
1070:
1059:
1050:
1047:Comet Wild 2
1042:
1036:
1034:
1027:
1026:CIDA of the
990:
974:
970:
965:
958:
952:
946:
902:
801:
794:
776:
772:
766:
753:
748:
740:
730:
723:
711:
707:
704:
698:
694:
689:
680:
676:
671:
667:
663:
649:
640:
629:
616:
603:
598:
596:
588:
582:
576:
550:
544:
535:
520:
513:
500:Comet Wild 2
489:
480:
468:John Simpson
461:
455:
453:
436:
428:
422:
415:
409:
407:
375:
371:COBE mission
352:
336:
330:
325:
321:
311:
292:
276:
264:
261:
234:
228:
224:
216:
213:
188:
173:
150:
124:
122:
114:
108:
102:
96:
65:
44:Solar System
36:Solar System
31:
30:
7552:Cosmic dust
7442:Altwegg, K.
7381:Altwegg, K.
7337:(A26): 14.
6800:: 149–160.
6537:Phaethon".
6248:: 209–212.
5957:26 February
5894:25 February
5832:25 February
5720:25 February
5673:25 February
5624:22 February
5575:22 February
5488:22 February
5442:19 February
4487:(1–4): 93.
4302:11 February
2283:11 February
2028:(7): 1243.
973:) and PIA (
719:channeltron
613:outer rings
597:During the
551:BepiColombo
417:Explorer 23
411:Explorer 16
267:microscopic
7541:Categories
7466:2012.01495
7398:(A32): 8.
7239:2010.13379
6924:11 October
6552:1904.07384
6447:"DESTINY+"
4964:(1): 243.
4904:2009.10377
4460:29 January
4396:23 January
4078:2304.00452
4025:(3): 291.
3887:(9): 967.
3840:(2): 236.
3786:(8): 144.
3641:(1): 719.
3594:(6): 741.
3494:(2): 420.
3159:(1): 298.
3117:(2): 180.
2719:23 January
2651:(1): 151.
2418:(2): 135.
1905:2012.08402
1871:5 February
1533:References
1474:reflectron
1417:missions.
1404:The first
1290:lunar soil
1202:paraboloid
1180:indicated.
983:Heidelberg
804:spacecraft
733:spacecraft
726:spacecraft
523:spacecraft
430:Pioneer 11
424:Pioneer 10
338:Pioneer 11
332:Pioneer 10
219:satellites
110:Vanguard 1
104:Explorer 1
80:atmosphere
76:meteoroids
68:space dust
25:spallation
7420:195549622
7359:182330353
7155:245366019
6975:128567869
6650:Canup, R.
6577:118708512
6545:: 22–42.
6384:242295026
6062:121243309
5771:124773731
5125:122405233
5068:186245081
5014:: 67–83.
4986:124533915
4929:225014796
4627:132133302
4103:237692026
3979:: 19177.
3808:230629869
3562:125115666
3408:122995125
3166:0704.2253
2460:. NASA TM
2218:(1): 31.
1942:234356185
1672:121139277
1429:Hayabusa2
1339:In 1950,
1334:Chang'e 5
1306:molecular
1302:elemental
1164:Enceladus
1118:≈ 20–50)
951:missions
917:ρ
886:≈
875:Δ
705:The twin
677:Pioneer 8
672:Pioneer 9
668:Pioneer 8
599:Voyager 2
590:Voyager 2
584:Voyager 1
225:Pioneer 8
116:Sputnik 3
94:meteors.
7024:51735815
6775:16578350
6682:11507633
6609:"IMPACT"
6469:DESTINY+
6451:DESTINY+
6431:3 August
6389:2 August
6337:2 August
6311:2 August
6306:27532569
6259:2 August
6221:2 August
6175:2 August
6170:22047326
6121:2 August
6116:19044367
6067:1 August
6013:1 August
5984:: 1043.
5952:24111692
5944:27081064
5881:21697830
5827:33554377
5819:16527969
5437:53122588
5382:37996161
5374:15205526
5314:: 1338.
4686:29545651
4563:26085272
4509:18649518
3462:20370201
3191:18970907
3066:17673274
3005:17833722
2776:35563939
2768:17733236
2613:: 1649.
2386:18698928
2364:(1): 1.
2337:27 April
2332:28372412
2237:27 April
2170:27 April
2165:22852725
2116:27 April
2111:21974623
2047:27 April
1968:27 April
1829:23 March
1780:21191301
1772:17754247
1496:See also
1419:Hayabusa
1414:Hayabusa
1406:asteroid
1382:Stardust
1372:flew by
1370:Stardust
1365:Stardust
1298:isotopic
1258:Geminids
1242:Japanese
1055:Tempel 1
1051:Stardust
1043:Stardust
1038:Stardust
1028:Stardust
1013:nitrogen
1005:hydrogen
491:Stardust
443:Saturn 1
355:infrared
329:and the
322:Helios 1
293:Columbia
62:Overview
7525:15 July
7516:Bibcode
7488:15 July
7471:Bibcode
7425:15 July
7400:Bibcode
7364:15 July
7339:Bibcode
7303:15 July
7284:Bibcode
7255:15 July
7205:12 July
7179:12 July
7133:Bibcode
7104:12 July
7077:Bibcode
7048:11 July
7002:Bibcode
6953:Bibcode
6907:Bibcode
6866:Bibcode
6837:10 July
6811:11 July
6802:Bibcode
6766:1063272
6743:Bibcode
6690:4413525
6662:Bibcode
6632:Bibcode
6615:. LASP.
6597:. LASP.
6557:Bibcode
6453:. JAXA.
6362:Bibcode
6250:Bibcode
6204:Bibcode
6150:Bibcode
6096:Bibcode
6042:Bibcode
5986:Bibcode
5924:Bibcode
5916:Science
5889:4400807
5861:Bibcode
5799:Bibcode
5791:Science
5749:Bibcode
5703:Bibcode
5656:Bibcode
5607:Bibcode
5558:Bibcode
5517:Bibcode
5471:Bibcode
5417:Bibcode
5387:29 July
5354:Bibcode
5346:Science
5325:29 July
5316:Bibcode
5274:Bibcode
5244:20 July
5239:4358568
5219:Bibcode
5187:20 July
5182:4349968
5162:Bibcode
5130:20 July
5105:Bibcode
5073:20 July
5048:Bibcode
5016:Bibcode
4966:Bibcode
4909:Bibcode
4867:29 June
4850:Bibcode
4821:18 June
4804:Bibcode
4775:18 June
4758:Bibcode
4720:Bibcode
4718:: 268.
4677:5846084
4654:Bibcode
4605:Bibcode
4571:4453018
4543:Bibcode
4489:Bibcode
4455:6788637
4435:Bibcode
4391:4315361
4371:Bibcode
4328:Bibcode
4285:Bibcode
4256:18 June
4239:Bibcode
4193:Bibcode
4137:Bibcode
4108:17 June
4083:Bibcode
4044:17 June
4027:Bibcode
3998:17 June
3981:Bibcode
3952:17 June
3935:Bibcode
3906:18 June
3889:Bibcode
3859:17 June
3842:Bibcode
3788:Bibcode
3758:15 June
3732:15 June
3701:4363877
3681:Bibcode
3643:Bibcode
3596:Bibcode
3542:Bibcode
3540:: 116.
3496:Bibcode
3442:Bibcode
3388:Bibcode
3386:: 278.
3311:Bibcode
3273:Bibcode
3171:Bibcode
3119:Bibcode
3046:Bibcode
2997:1739199
2977:Bibcode
2969:Science
2936:Bibcode
2934:: 617.
2880:Bibcode
2848:Bibcode
2810:Bibcode
2808:: 185.
2748:Bibcode
2740:Science
2702:Bibcode
2653:Bibcode
2615:Bibcode
2577:Bibcode
2575:: 841.
2548:5 March
2531:Bibcode
2502:5 March
2493:Bibcode
2464:4 March
2420:Bibcode
2366:Bibcode
2312:Bibcode
2266:Bibcode
2220:Bibcode
2145:Bibcode
2091:Bibcode
2030:Bibcode
1995:: 208.
1910:Bibcode
1852:Bibcode
1785:2 March
1752:Bibcode
1744:Science
1723:2 March
1706:Bibcode
1677:2 March
1652:Bibcode
1623:2 March
1614:Bibcode
1585:2 March
1580:4206906
1560:Bibcode
1482:Rosetta
1455:Rosetta
1446:Rosetta
1378:aerogel
1250:DESTINY
1190:Cassini
1160:Cassini
1152:Cassini
1144:Jupiter
1108:mission
1106:Cassini
1094:quinone
1060:Ulysses
993:≈ 100)
907:density
777:Ulysses
773:Galileo
754:Galileo
749:Ulysses
741:Galileo
731:Ulysses
724:Galileo
712:Ulysses
708:Galileo
699:Ulysses
695:Galileo
659:Jupiter
634:by the
625:Neptune
617:Voyager
605:Cassini
555:Mercury
549:of the
545:On the
217:Pegasus
99:bullets
7418:
7357:
7201:. NASA
7175:. NASA
7153:
7095:
7044:. NASA
7022:
6973:
6833:. NASA
6773:
6763:
6714:8 July
6710:. NASA
6688:
6680:
6654:Nature
6591:"IDEX"
6575:
6471:. DLR.
6427:. NASA
6382:
6304:
6294:
6168:
6114:
6060:
6004:
5950:
5942:
5887:
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