scholarly journals Light Scattering by Dust Particles in the Outer Solar System

1991 ◽  
Vol 126 ◽  
pp. 155-158
Author(s):  
J.W. Hovenier ◽  
P.B. Bosma
Keyword(s):  
Solar System ◽  
Cross Section ◽  
Particle Density ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Outer Solar System ◽  
Zodiacal Light ◽  
Particle Density Distribution ◽  
Photometric Observations ◽  
Pioneer 10

AbstractPhotometric observations of the zodiacal light performed by Pioneer 10 indicated that there may be very little scattering by dust in the outer solar system. To shed more light on this problem we formulate explicit expressions for interpreting the brightness observed by a spacecraft travelling inside or outside a finite homogeneous cloud of scattering particles. An application is made to the ecliptic zodiacal light brightness as observed by Pioneer 10 and tabulated by Toller and Weinberg (1985). A satisfactory interpretation of these data as well as earthbound observations can be given by means of a model having a particle density distribution or mean scattering cross section which vanishes beyond 2.8 - 3.7 AU. Some implications for the nature and spatial distribution of the interplanetary dust are discussed.

scholarly journals Dust Measurements in the Outer Solar System

1994 ◽  
Vol 160 ◽  
pp. 367-380
Author(s):  
Eberhard Grün
Keyword(s):  
Solar System ◽  
Interstellar Dust ◽  
Thermal Emission ◽  
Scattered Light ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Spatial Density ◽  
Outer Solar System ◽  
The Sun

In-situ measurements of micrometeoroids provide information on the spatial distribution of interplanetary dust and its dynamical properties. Pioneers 10 and 11, Galileo and Ulysses spaceprobes took measurements of interplanetary dust from 0.7 to 18 AU distance from the sun. Distinctly different populations of dust particles exist in the inner and outer solar system. In the inner solar system, out to about 3 AU, zodiacal dust particles are recognized by their scattered light, their thermal emission and by in-situ detection from spaceprobes. These particles orbit the sun on low inclination (i ≤ 30°) and moderate eccentricity (e ≤ 0.6) orbits. Their spatial density falls off with approximately the inverse of the solar distance. Dust particles on high inclination or even retrograde trajectories dominate the dust population outside about 3 AU. The dust detector on board the Ulysses spaceprobe identified interstellar dust sweeping through the outer solar system on hyperbolic trajectories. Within about 2 AU from Jupiter Ulysses discovered periodic streams of dust particles originating from within the jovian system.

scholarly journals The Contribution of Kuiper Belt Dust Grains to the Inner Solar System

1996 ◽  
Vol 150 ◽  
pp. 163-166
Author(s):  
Jer-Chyi Liou ◽  
Herbert A. Zook ◽  
Stanley F. Dermott
Keyword(s):  
Solar System ◽  
Interstellar Dust ◽  
Numerical Study ◽  
Kuiper Belt ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Dust Grains ◽  
Zodiacal Light ◽  
Interplanetary Dust Particles ◽  
The Earth

AbstractThe recent discovery of the so-called Kuiper belt objects has prompted the idea that these objects produce dust grains that may contribute significantly to the interplanetary dust population at 1 AU. We have completed a numerical study of the orbital evolution of dust grains, of diameters 1 to 9 μm, that originate in the region of the Kuiper belt. Our results show that about 80% of the grains are ejected from the Solar System by the giant planets while the remaining 20% of the grains evolve all the way to the Sun. Surprisingly, these dust grains have small orbital eccentricities and inclinations when they cross the orbit of the Earth. This makes them behave more like asteroidal than cometary-type dust particles. This also enhances their chances to be captured by the Earth and makes them a possible source of the collected interplanetary dust particles (IDPs); in particular, they represent a possible source that brings primitive/organic materials from the outer Solar System to the Earth.When collisions with interstellar dust grains are considered, however, Kuiper belt dust grains larger than about 9 μm appear likely to be collisionally shattered before they can evolve to the inner part of the Solar System. Therefore, Kuiper belt dust grains may not, as they are expected to be small, contribute significantly to the zodiacal light.

scholarly journals Evidence that the Properties of Interplanetary Dust Beyond 1 AU are Not Homogeneous

1980 ◽  
Vol 90 ◽  
pp. 71-74 ◽  
Author(s):  
Donald W. Schuerman
Keyword(s):  
Cross Section ◽  
Heliocentric Distance ◽  
Interplanetary Dust ◽  
Scattering Cross Section ◽  
Zodiacal Light ◽  
Dust Density ◽  
Scattering Cross ◽  
Pioneer 10

Traditionally, earth-based observations of the zodiacal light (ZL) require two assumptions for further analysis: (A1) the dust density (n) is a power of heliocentric distance (R), n ∝ R−ν; (A2) the nature (scattering cross section, σ) of the dust is independent of location, σ(r,h,θ)=σ(θ). Observations from Pioneer 10 do not verify these assumptions.

scholarly journals Physical Modeling of the Zodiacal Dust Cloud

2001 ◽  
Vol 204 ◽  
pp. 17-34 ◽  
Author(s):  
Leonid M. Ozernoy
Keyword(s):  
Solar System ◽  
Physical Modeling ◽  
Interstellar Dust ◽  
Extrasolar Planets ◽  
Dust Cloud ◽  
Interplanetary Dust ◽  
Asteroid Belt ◽  
Dust Particles ◽  
Resonant Structure ◽  
Zodiacal Light

This review is based on extensive work done in collaboration with N. Gorkavyi, J. Mather, and T. Taidakova, which aimed at physical modeling of the interplanetary dust (IPD) cloud in the Solar System, i.e., establishing a link between the observable characteristics of the zodiacal cloud and the dynamical and physical properties of the parent minor bodies. Our computational approach permits one to integrate the trajectories of hundreds of particles and to effectively store up to 1010–11 positions with modest computer resources, providing a high fidelity 3D distribution of the dust. Our numerical codes account for the major dynamical effects that govern the motion of IPD particles: Poynting-Robertson (P-R) drag and solar wind drag; solar radiation pressure; particle evaporation; gravitational scattering by the planets; and the influence of mean-motion resonances. The incorporation of secular resonances and collisions of dust particles (both mutual and with interstellar dust) is underway. We have demonstrated the efficacy of our codes by performing the following analyses: (i) simulation of the distribution of Centaurs (comets scattered in their journey from the Kuiper belt inward in the Solar System) and revealing the effects of the outer planets in producing ‘cometary belts’; (ii) detailed inspection of a rich resonant structure found in these belts, which predicts the existence of gaps similar to the Kirkwood gaps in the main asteroid belt; (iii) a preliminary 3-D physical model of the IPD cloud, which includes three dust components – asteroidal, cometary, and kuiperoidal – and is consistent with the available data of Pioneer and Voyager dust detectors; (iv) modeling of the IPD cloud, which provides a zodiacal light distribution in accord, to the order of 1%, with a subset of the COBE/DIRBE observations; and (v) showing that the resonant structure in dusty circumstellar disks of Vega and Epsilon Eridani is a signature of embedded extrasolar planets. Further improvements of our modeling and their importance for astronomy and cosmology are outlined.

Planetary Compositions - Clues from Meteorites and Asteroids

1989 ◽  
Vol 44 (10) ◽  
pp. 924-934 ◽  
Author(s):  
Edward R. D. Scott ◽  
Horton E. Newsom
Keyword(s):  
High Temperature ◽  
Solar System ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Outer Solar System ◽  
The Sun ◽  
Interplanetary Dust Particles ◽  
Comet Halley ◽  
As Effects ◽  
System Chemistry

Abstract We review the chemical and mineralogical properties of primitive meteorites and chemical data for the Sun, Comet Halley and interplanetary dust particles. Regardless of where meteorites formed, concentrations of rock-forming elements in solar nebular solids could not have varied simply with distance from the Sun. Thus compositional differences between neighboring planets and the chemical and mineralogical diversity of chondritic asteroids may have been caused by local variations in the compositions of planetesimals, rather than transport of planetesimals over large heliocentric dis­ tances. Chemical variations were partly caused by differential transport and preferential agglomer­ ation of various presolar and solar grains and aggregates, and the production from these aggregates of diverse types of chondrules, refractory inclusions and other chondritic components in brief, local high temperature events in the nebula. These processes were just as important in controlling solar system chemistry as effects due to changes in ambient nebular temperatures and pressures. Differ­ ences between the Fe/Si ratios of the Sun, CI chondrites, interplanetary dust particles and Comet Halley suggest that planetesimals in the outer solar system had diverse relative concentrations of rock-forming elements.

scholarly journals Analogues of interplanetary dust particles to interpret the zodiacal light polarization

2020 ◽  
Vol 183 ◽  
pp. 104527 ◽  
Author(s):  
E. Hadamcik ◽  
J. Lasue ◽  
A.C. Levasseur-Regourd ◽  
J.-B. Renard
Keyword(s):  
Interplanetary Dust ◽  
Light Polarization ◽  
Dust Particles ◽  
Zodiacal Light ◽  
Interplanetary Dust Particles

scholarly journals The Optical Properties of Interplanetary Dust

1991 ◽  
Vol 126 ◽  
pp. 163-170 ◽  
Author(s):  
P.L. Lamy ◽  
J.M. Perrin
Keyword(s):  
Optical Properties ◽  
Light Scattering ◽  
Phase Function ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Local Enhancement ◽  
Zodiacal Light ◽  
Laboratory Results

AbstractAfter briefly evaluating the observations of the Zodiacal Light and F-corona, we review the laboratory results on the light scattering by dust particles and the various theories which have been recently proposed. We then discuss the optical properties of the dust with emphasis on the phase function, the polarization, the color, the albedo and the local enhancement in the Gegenschein.

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.

scholarly journals Far-ultraviolet Studies. VIII. Apollo 17 Search for Zodiacal Light

1980 ◽  
Vol 90 ◽  
pp. 41-44
Author(s):  
R. C. Henry ◽  
R. C. Anderson ◽  
W. G. Fastie
Keyword(s):  
Solar System ◽  
Dust Particles ◽  
Zodiacal Light ◽  
The Past ◽  
Far Ultraviolet

Solar System dust particles reflect sunlight, producing the so-called zodiacal light (Leinert 1975). The spectrum of the zodiacal light in the far ultraviolet has been a matter of controversy in the past, and remains a subject of great interest.

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