scholarly journals Cosmic Dust in the Atmosphere and in the Interplanetary Space at 1 AU Today and in the Early Solar System

1971 ◽  
Vol 13 ◽  
pp. 209-221 ◽  
Author(s):  
H. Fechtig
Keyword(s):  
Solar System ◽  
Interplanetary Space ◽  
Cosmic Dust ◽  
Dust Particles ◽  
Early Solar System ◽  
Lunar Samples ◽  
Order Of Magnitude ◽  
Flux Model ◽  
Variable Flux ◽  
Ionization Detectors

Reliable measurements of cosmic dust abundances have been obtained by ionization detectors during particle impact and by collectors controlled either by inflight shadowing or by penetration-hole identification. A description of the techniques used is given.Crater-number densities observed on the lunar surface and on lunar samples represent an important source of information on cosmic dust fluxes. The related results from the Apollo 11 and 12 missions are reviewed. The overall knowledge gained from these measurements leads to the following flux model: The cumulative flux Φ vs mass m follows the extrapolation from larger meteoroid-size range (Watson’s Law) and can be described byThe Pioneer 8 dust experiment and lunar samples indicate a depletion of the flux at approximately 10-8g. However, cosmic dust particles exist in interplanetary space at least down to 0.3 μ. diameter. They are interpreted as nonmetallic particles in the solar system.The atmosphere shows an enhancement in particles of about one order of magnitude compared to the flux in interplanetary space at 1 AU. No depletion or cutoff could be detected. These particles are interpreted as lunar debris or as disintegrated products from fireballs.The numbers of large lunar craters (>140 m diameter) in Mare Tranquillitatis and in Oceanus Procellarum are compared with the meteoroid flux. These comparisons lead to a time-variable flux of Φ.e-Bt, with B = 2.6 and t = time in 109 yr. Thus, the meteoroidflux at the formation of the lunar maria was approximately 4 orders of magnitude higher than today.

scholarly journals Dust Around Young Stars: How Related to Solar System Dust?

1995 ◽  
Vol 10 ◽  
pp. 351-392 ◽  
Author(s):  
Martha S. Hanner
Keyword(s):  
Solar System ◽  
Interplanetary Space ◽  
Circumstellar Disks ◽  
Theoretical Work ◽  
Interplanetary Dust ◽  
Young Stars ◽  
Dust Particles ◽  
Interplanetary Dust Particles ◽  
Technical Advances ◽  
Dust Disks

Study of the dust in circumstellar disks around young stars is currently an extremely active area in astronomy. There is little doubt that accretion disks are a natural part of protostellar evolution. Much recent observational and theoretical work is giving us a clearer picture of the physical conditions in dust disks and their evolutionary progression. IRAS observations revealed that many main-sequence stars, such as p Pictoris, have circumstellar disks. But whether these disks are related to planetary formation is not yet understood.A portion of the dust in disks around young stars ultimately may be incorporated into planetary systems. Thus, study of the dust in our own solar system complements the remote sensing of protostellar regions and aids in reconstructing the evolutionary history of the dust. Since comets formed in the cold outer regions of the solar nebula, they may contain intact interstellar grains. As the comets lose material during passage through the warm inner solar system, some of these grains will be released into interplanetary space. Technical advances now allow analysis of individual micrometer or smaller grains in interplanetary dust particles and primitive meteorite samples. Isotopic anomalies and patterns of crystal growth in these particles are yielding tantalizing clues about the interstellar material incorporated into these solar system samples.

Collection alteration and pristine structural properties of dust particles collected by MIDAS/Rosetta at comet 67P/Churyumov-Gerasimenko

2021 ◽  
Author(s):  
Minjae Kim ◽  
Thurid Mannel ◽  
Jeremie Lasue ◽  
Mark Bentely ◽  
Richard Moissl
Keyword(s):  
Solar System ◽  
Structural Properties ◽  
Shape Descriptor ◽  
Planetary Science ◽  
Dust Particles ◽  
Early Solar System ◽  
Cometary Dust ◽  
Major Alteration ◽  
Analysis System ◽  
Comet 67P

<p>Comets are believed to have preserved pristine material from the early stages of the Solar System formation, thus providing unique information on intricate processes like dust growth mechanisms. The Rosetta mission gave us the best opportunity to investigate nearly pristine cometary dust particles of comet 67P/Churyumov–Gerasimenko. Among the three in-situ dust instruments, the MIDAS (Micro-Imaging Dust Analysis System) atomic force microscope collected cometary dust particles with sizes from hundreds of nanometres to tens of micrometres and recorded their 3D topography, size, shape, morphology, and related parameters [1].</p> <p>MIDAS collected dust emitted from comet 67P on dedicated targets. Particles fell through the entry funnel and collided with the collection targets [2] causing an unknown degree of particle alteration. To understand which structural properties of the dust remained pristine and can be used to understand comets and early Solar System processes it is important to understand the collection alteration. Dedicated laboratory experiments were carried out by previous studies [3, 4]. They found that the degree of alteration upon collection is strongly determined by the particle size, strength, and the collection velocity. They indicate that particles in the MIDAS size range deposited with moderate velocities about less than a few metres per second can stick on a target without major alteration.</p> <p>We aim to determine the structurally least altered MIDAS particles and investigate their properties. As database we use an improved version of the MIDAS particle catalogue [5]. Selecting all particles suitable for our analysis (e.g., cometary origin, sufficiently high image quality) grants us topographic data of over 600 nano- to micrometre-sized dust particles of comet 67P. We create dust coverage maps showing the distribution of the selected dust particles on the collection targets. As first, simple classification we divide the particles into those detected in clusters, suggested to be fragments originating in a shattering event of one large parent particle, and those remote from others that are potentially individually collected particles. Finally, we use a shape descriptor to categorise the particles according to their characteristics, e.g., shape and size, and compare to previous results from COSIMA [6] and simulation/laboratory studies [3, 7].</p> <p> </p> <p>[1] Bentley, M.S., Schmied, R., Mannel, T., et al. 2016, Nature, 537</p> <p>[2] Bentley, M. S., Arends, H., Butler, B., et al. 2016, Acta Astronautica, 125, 11</p> <p>[3] Ellerbroek, L. E., Gundlach, B., Landeck, A., et al. 2017, MNRAS, 469, S204</p> <p>[4] Ellerbroek, L. E., Gundlach, B., Landeck, A., et al. 2019, MNRAS, 486, S3755</p> <p>[5] Boakes, P., and the MIDAS team, 2018. ‘MIDAS Particle Catalogue’. ESA Planetary Science Archive  Dataset: RO-C-MIDAS-5-PRL-TO-EXT3-V2.0. Product ID: RO-C-MIDAS-5-PRL-TO-EXT3-V2.0</p> <p>[6] Langevin, Y., Hilchenbach, M., Ligier, N., et al. 2016, Icarus, 271, 76</p> <p>[7] Lasue, J., Maroger, I., Botet, R., et al. 2019, A&A, 630,</p>

scholarly journals The Present Status of the Munich Dust Counter Experiment on Board of the Hiten Spacecraft

1991 ◽  
Vol 126 ◽  
pp. 15-20 ◽  
Author(s):  
E. Igenbergs ◽  
A. Hüdepohl ◽  
K. Uesugi ◽  
T. Hayashi ◽  
H. Svedhem ◽  
...  
Keyword(s):  
Solar System ◽  
Present Status ◽  
Cosmic Dust ◽  
Dust Particles ◽  
Preliminary Results ◽  
Scientific Experiment ◽  
Directional Distributions

AbstractThe Munich Dust Counter (MDC) is a scientific experiment on board the MUSES-A mission of Japan measuring cosmic dust. The satellite HITEN of this mission has been launched on January 24th, 1990 from Kagoshima Space Center. Here the present status of the MDC experiment is summarized. The number of dust particles measured so far is presented together with first and preliminary results of flux calculations and spatial as well as directional distributions of cosmic dust particles measured until July 25, 1990. A clear evidence of particles coming from the inner solar system (beta-meteoroids) already has been found. These are compared to particles coming from the apex direction.

scholarly journals Observational constraints on the likelihood of 26Al in planet-forming environments

2020 ◽  
Vol 644 ◽  
pp. L1
Author(s):  
Megan Reiter
Keyword(s):  
Solar System ◽  
Planet Formation ◽  
Radioactive Decay ◽  
High Mass ◽  
Mass Star ◽  
Early Solar System ◽  
Star Forming ◽  
Star Forming Regions ◽  
The Galaxy ◽  
Order Of Magnitude

Recent work suggests that 26Al may determine the water budget in terrestrial exoplanets as its radioactive decay dehydrates planetesimals leading to rockier compositions. Here I consider the observed distribution of 26Al in the Galaxy and typical star-forming environments to estimate the likelihood of 26Al enrichment during planet formation. I do not assume Solar-System-specific constraints as I am interested in enrichment for exoplanets generally. Observations indicate that high-mass stars dominate the production of 26Al with nearly equal contributions from their winds and supernovae. Observed 26Al abundances are comparable to those in the early Solar System in the high-mass star-forming regions where most stars (and thereby most planets) form. These high abundances appear to be maintained for a few million years, which is much longer than the 0.7 Myr half-life. Observed bulk 26Al velocities are an order of magnitude slower than expected from winds and supernovae. These observations are at odds with typical model assumptions that 26Al is provided instantaneously by high velocity mass loss from supernovae and winds. The regular replenishment of 26Al, especially when coupled with the small age differences that are common in high-mass star-forming complexes, may significantly increase the number of star- and planet-forming systems exposed to 26Al. Exposure does not imply enrichment, but the order of magnitude slower velocity of 26Al may alter the fraction that is incorporated into planet-forming material. Together, this suggests that the conditions for rocky planet formation are not rare, nor are they ubiquitous, as small regions such as Taurus, that lack high-mass stars to produce 26Al may be less likely to form rocky planets. I conclude with suggested directions for future studies.

scholarly journals The asteroid-comet continuum from laboratory and space analyses of comet samples and micrometeorites

2015 ◽  
Vol 11 (A29A) ◽  
pp. 253-256 ◽  
Author(s):  
Cécile Engrand ◽  
Jean Duprat ◽  
Noémie Bardin ◽  
Emmanuel Dartois ◽  
Hugues Leroux ◽  
...  
Keyword(s):  
Solar System ◽  
Interplanetary Dust ◽  
Cosmic Dust ◽  
Dust Particles ◽  
Interplanetary Dust Particles ◽  
Cometary Dust ◽  
History Of ◽  
Polar Snow ◽  
Comet 67P ◽  
Cometary Origin

AbstractComets are probably the best archives of the nascent solar system, 4.5 Gyr ago, and their compositions reveal crucial clues on the structure and dynamics of the early protoplanetary disk. Anhydrous minerals (olivine and pyroxene) have been identified in cometary dust for a few decades. Surprisingly, samples from comet Wild2 returned by the Stardust mission in 2006 also contain high temperature mineral assemblages like chondrules and refractory inclusions, which are typical components of primitive meteorites (carbonaceous chondrites - CCs). A few Stardust samples have also preserved some organic matter of comet Wild 2 that share some similarities with CCs. Interplanetary dust falling on Earth originate from comets and asteroids in proportions to be further constrained. These cosmic dust particles mostly show similarities with CCs, which in turn only represent a few percent of meteorites recovered on Earth. At least two (rare) families of cosmic dust particles have shown strong evidences for a cometary origin: the chondritic porous interplanetary dust particles (CP-IDPs) collected in the terrestrial stratosphere by NASA, and the ultracarbonaceous Antarctic Micrometeorites (UCAMMs) collected from polar snow and ice by French and Japanese teams. Analyses of dust particles from the Jupiter family comet 67P/Churyumov-Gerasimenko by the dust analyzers on Rosetta orbiter (COSIMA, GIADA, MIDAS) suggest a relationship to interplanetary dust/micrometeorites. A growing number of evidences highlights the existence of a continuum between asteroids and comets, already in the early history of the solar system.

scholarly journals 5.7 Rotational Bursting of Interplanetary Dust Particles

1976 ◽  
Vol 31 ◽  
pp. 453-457
Author(s):  
Stephen J. Paddack ◽  
John W. Rhee
Keyword(s):  
Solar System ◽  
Solar Radiation Pressure ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
High Resistivity ◽  
Interplanetary Dust Particles ◽  
Metallic Particles ◽  
Order Of Magnitude ◽  
Magnetic Spin ◽  
Iron Nickel

AbstractSolar radiation pressure can cause rotational bursting and eventual elimination from the solar system of small asymmetric interplanetary particles by a windmill effect. The life span determined by this process for stony meteoritic material or tektite glass with radii of 1 cm is on the order of 105 years. Same size material which contains iron, nickel or aluminum, with properties such that it is subject to 5 percent of the amount of spin damping as pure metals, can be removed from the solar system on the order of 106 years by this process. Ordinary chondritic material, despite its high resistivity, is subject to a type of magnetic spin damping, in addition to the normal spin damping, with the consequent result that this type material cannot be removed from the solar system by this process. This depletion mechanism appears to work faster than the traditional Poynting-Robertson effect by approximately two orders of magnitude for the nonmetallic particles and one order of magnitude for the metallic particles.

Transmission Electron Microscopy Studies of Natural Nanomaterials from the Solar System

2000 ◽  
Vol 6 (S2) ◽  
pp. 412-413
Author(s):  
Z. R. Dai ◽  
J. P. Bradley ◽  
T. P. Snow ◽  
Z. L Wang
Keyword(s):  
Solar System ◽  
Materials Science ◽  
Interplanetary Space ◽  
Interplanetary Dust ◽  
Planetary Science ◽  
Mass Spectrometry Data ◽  
Dust Particles ◽  
Interplanetary Dust Particles ◽  
New Frontier ◽  
Individual Grains

It is widely appreciated that the study of (man-made) nanomaterials is a new frontier in materials science, but it is not well appreciated that (natural) nanomaterials represent a new frontier in meteoritics and planetary science [1]. During the next decade the nanogram to microgram quantities of extraterrestrial materials will be returned to Earth from a variety of solar system bodies including comets [2]. Studies of cometary interplanetary dust particles (IDPs) collected in the stratosphere, as well as mass spectrometry data from grains analyzed in-situ at comet Halley, suggest that the returned comet samples will be heterogeneous on a scale of nanometers [3, 4]. (A single 5-10μm diameter IDP may contain >106 individual grains and many different minerals (metal, carbonaceous phases, silicates, sulfides, etc.)). More recent observations of dust around stars, in interplanetary space, and at comet Hale-Bopp indicate that the predominant astronomical grain size is in the nanometer to submicrometer size range [5,6].

Composition of Cosmic Dust: Sources and Implications for the Early Solar System

Elements ◽  
2016 ◽  
Vol 12 (3) ◽  
pp. 177-183 ◽  
Author(s):  
George J. Flynn ◽  
Larry R. Nittler ◽  
Cécile Engrand
Keyword(s):  
Solar System ◽  
Cosmic Dust ◽  
Early Solar System ◽  
Dust Sources

scholarly journals What can pre-solar grains tell us about the solar nebula?

2006 ◽  
Vol 2 (14) ◽  
pp. 353-356 ◽  
Author(s):  
Gary R. Huss ◽  
Bruce T. Draine
Keyword(s):  
Solar System ◽  
Solar Nebula ◽  
Interplanetary Dust ◽  
Radiation Environment ◽  
Dust Particles ◽  
Early Solar System ◽  
Interplanetary Dust Particles ◽  
Fine Grained ◽  
Isotopic Compositions ◽  
Relative Abundances

AbstractSeveral types of pre-solar grains, grains that existed prior to solar system formation, have been found in the fine-grained components of primitive meteorites, interplanetary dust particles (IDPs), and comet samples. Known pre-solar components have isotopic compositions that reflect formation from the ejecta of evolved stars. Other pre-solar materials may have isotopic compositions very similar to solar system materials, making their identification as pre-solar grains problematic. Pre-solar materials exhibit a range of chemical and thermal resistance, so their relative abundances can be used to probe the conditions in the solar nebula. Detailed information on the relative abundances of pre-solar and solar-system materials can provide information on the temperatures, radiation environment, and degree of radial mixing in the early solar system.

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