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Andrew R. Poppe - One of the best experts on this subject based on the ideXlab platform.
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The contribution of Centaur-emitted Dust to the Interplanetary Dust distribution
Monthly Notices of the Royal Astronomical Society, 2019Co-Authors: Andrew R. PoppeAbstract:ABSTRACT Interplanetary Dust grains originate from a variety of source bodies, including comets, asteroids, and Edgeworth–Kuiper belt objects. Centaurs, generally defined as those objects with orbits that cross the outer planets, have occasionally been observed to exhibit cometary-like outgassing at distances beyond Jupiter, implying that they may be an important source of Dust grains in the outer Solar system. Here, we use an Interplanetary Dust grain dynamics model to study the behaviour and equilibrium distribution of Centaur-emitted Interplanetary Dust grains. We focus on the five Centaurs with the highest current mass-loss rates: 29P/Schwassmann-Wachmann 1, 166P/2001 T4, 174P/Echeclus, C/2001 M10, and P/2004 A1, which together comprise 98 per cent of the current mass loss from all Centaurs. Our simulations show that Centaur-emitted Dust grains with radii s < 2 μm have median lifetimes consistent with Poynting–Robertson (P–R) drag lifetimes, while grains with radii s > 2 μm have median lifetimes much shorter than their P–R drag lifetimes, suggesting that dynamical interactions with the outer planets are effective in scattering larger grains, in analogy to the relatively short lifetimes of Centaurs themselves. Equilibrium density distributions of grains emitted from specific Centaurs show a variety of structure including local maxima in the outer Solar system and azimuthal asymmetries, depending on the orbital elements of the parent Centaur. Finally, we compare the total Centaur Interplanetary Dust density to Dust produced from Edgeworth–Kuiper belt objects, Jupiter-family comets, and Oort cloud comets, and conclude that Centaur-emitted Dust may be an important component between 5 and 15 au, contributing approximately 25 per cent of the local Interplanetary Dust density at Saturn.
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Interplanetary Dust, Meteoroids, Meteors and Meteorites
Space Science Reviews, 2019Co-Authors: Detlef Koschny, Jérémie Lasue, Anny Chantal Levasseur-regourd, George J. Flynn, Rachel H. Soja, Cecile Engrand, David Malaspina, Tomoki Nakamura, Andrew R. Poppe, Veerle J. SterkenAbstract:Interplanetary Dust particles and meteoroids mostly originate from comets and asteroids. Understanding their distribution in the Solar system, their dynamical behavior and their properties, sheds light on the current state and the dynamical behavior of the Solar system. Dust particles can endanger Earth-orbiting satellites and deep-space probes, and a good understanding of the spatial density and velocity distribution of Dust and meteoroids in the Solar system is important for designing proper spacecraft shielding. The study of Interplanetary Dust and meteoroids provides clues to the formation of the Solar system. Particles having formed 4.5 billion years ago can survive planetary accretion and those that survived until now did not evolve significantly since then. Meteoroids and Interplanetary Dust can be observed by measuring the intensity and polarization of the zodiacal light, by observing meteors entering the Earth’s atmosphere, by collecting them in the upper atmosphere, polar ices and snow, and by detecting them with in-situ detectors on space probes.
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Interplanetary Dust, Meteoroids, Meteors and Meteorites
Space Science Reviews, 2019Co-Authors: Detlef Koschny, Jérémie Lasue, Anny Chantal Levasseur-regourd, George J. Flynn, Rachel H. Soja, Cecile Engrand, David Malaspina, Tomoki Nakamura, Andrew R. Poppe, Veerle J. SterkenAbstract:Interplanetary Dust particles and meteoroids mostly originate from comets and asteroids. Understanding their distribution in the Solar system, their dynamical behavior and their properties, sheds light on the current state and the dynamical behavior of the Solar system. Dust particles can endanger Earth-orbiting satellites and deep-space probes, and a good understanding of the spatial density and velocity distribution of Dust and meteoroids in the Solar system is important for designing proper spacecraft shielding. The study of Interplanetary Dust and meteoroids provides clues to the formation of the Solar system. Particles having formed 4.5 billion years ago can survive planetary accretion and those that survived until now did not evolve significantly since then. Meteoroids and Interplanetary Dust can be observed by measuring the intensity and polarization of the zodiacal light, by observing meteors entering the Earth’s atmosphere, by collecting them in the upper atmosphere, polar ices and snow, and by detecting them with in-situ detectors on space probes.
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Interplanetary Dust delivery of water to the atmospheres of Pluto and Triton
Astronomy & Astrophysics, 2018Co-Authors: Andrew R. Poppe, Mihaly HoranyiAbstract:Context. Both Pluto and Triton possess thin, N2-dominated atmospheres controlled by sublimation of surface ices. Aims. We aim to constrain the influx and ablation of Interplanetary Dust grains into the atmospheres of both Pluto and Triton in order to estimate the rate at which oxygen-bearing species are introduced into both atmospheres. Methods. We use (i) an Interplanetary Dust dynamics model to calculate the flux and velocity distributions of Interplanetary Dust grains relevant for both Pluto and Triton and (ii) a model for the ablation of Interplanetary Dust grains in the atmospheres of both Pluto and Triton. We sum the individual ablation profiles over the incoming mass and velocity distributions of Interplanetary Dust grains in order to determine the vertical structure and net deposition of water to both atmospheres. Results. Our results show that <2% of silicate grains ablate at either Pluto or Triton while approximately 75% and >99% of water ice grains ablate at Pluto and Triton, respectively. From ice grains, we calculate net water influxes to Pluto and Triton of ~3.8 kg day−1 (8.5 × 103 H2O cm−2 s−1) and ~370 kg day−1 (6.2 × 105 H2O cm−2 s−1), respectively. The significant difference in total water deposition between Pluto and Triton is due to the presence of Triton within Neptune’s gravity well, which both enhances Interplanetary Dust particle (IDP) fluxes due to gravitational focusing and accelerates grains before entry into Triton’s atmosphere, thereby causing more efficient ablation. Conclusions. We conclude that water deposition from Dust ablation plays only a minor role at Pluto due to its relatively low flux. At Triton, water deposition from IDPs is more significant and may play a role in the alteration of atmospheric and ionospheric chemistry. We also suggest that meteoric smoke and smaller, unablated grains may serve as condensation nuclei for the formation of hazes at both worlds.
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An improved model for Interplanetary Dust fluxes in the outer Solar System
Icarus, 2016Co-Authors: Andrew R. PoppeAbstract:Abstract We present an improved model for Interplanetary Dust grain fluxes in the outer Solar System constrained by in situ Dust density observations. A dynamical Dust grain tracing code is used to establish relative Dust grain densities and three-dimensional velocity distributions in the outer Solar System for four main sources of Dust grains: Jupiter-family comets, Halley-type comets, Oort-Cloud comets, and Edgeworth-Kuiper Belt objects. Model densities are constrained by in situ Dust measurements by the New Horizons Student Dust Counter, the Pioneer 10 meteoroid detector, and the Galileo Dust Detection System (DDS). The model predicts that Jupiter-family comet grains dominate the Interplanetary Dust grain mass flux inside approximately 10 AU, Oort-Cloud cometary grains may dominate between 10 and 25 AU, and Edgeworth-Kuiper Belt grains are dominant outside 25 AU. The model also predicts that while the total Interplanetary mass flux at Jupiter roughly matches that inferred by the analysis of the Galileo DDS measurements, mass fluxes to Saturn, Uranus, and Neptune are at least one order-of-magnitude lower than that predicted by extrapolations of Dust grain flux models from 1 AU. Finally, we compare the model predictions of Interplanetary Dust oxygen influx to the giant planet atmospheres with various observational and photochemical constraints and generally find good agreement, with the exception of Jupiter, which suggests the possibility of additional chemical pathways for exogenous oxygen in Jupiter’s atmosphere.
Anny Chantal Levasseur-regourd - One of the best experts on this subject based on the ideXlab platform.
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Interplanetary Dust, Meteoroids, Meteors and Meteorites
Space Science Reviews, 2019Co-Authors: Detlef Koschny, Jérémie Lasue, Anny Chantal Levasseur-regourd, George J. Flynn, Rachel H. Soja, Cecile Engrand, David Malaspina, Tomoki Nakamura, Andrew R. Poppe, Veerle J. SterkenAbstract:Interplanetary Dust particles and meteoroids mostly originate from comets and asteroids. Understanding their distribution in the Solar system, their dynamical behavior and their properties, sheds light on the current state and the dynamical behavior of the Solar system. Dust particles can endanger Earth-orbiting satellites and deep-space probes, and a good understanding of the spatial density and velocity distribution of Dust and meteoroids in the Solar system is important for designing proper spacecraft shielding. The study of Interplanetary Dust and meteoroids provides clues to the formation of the Solar system. Particles having formed 4.5 billion years ago can survive planetary accretion and those that survived until now did not evolve significantly since then. Meteoroids and Interplanetary Dust can be observed by measuring the intensity and polarization of the zodiacal light, by observing meteors entering the Earth’s atmosphere, by collecting them in the upper atmosphere, polar ices and snow, and by detecting them with in-situ detectors on space probes.
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Interplanetary Dust, Meteoroids, Meteors and Meteorites
Space Science Reviews, 2019Co-Authors: Detlef Koschny, Jérémie Lasue, Anny Chantal Levasseur-regourd, George J. Flynn, Rachel H. Soja, Cecile Engrand, David Malaspina, Tomoki Nakamura, Andrew R. Poppe, Veerle J. SterkenAbstract:Interplanetary Dust particles and meteoroids mostly originate from comets and asteroids. Understanding their distribution in the Solar system, their dynamical behavior and their properties, sheds light on the current state and the dynamical behavior of the Solar system. Dust particles can endanger Earth-orbiting satellites and deep-space probes, and a good understanding of the spatial density and velocity distribution of Dust and meteoroids in the Solar system is important for designing proper spacecraft shielding. The study of Interplanetary Dust and meteoroids provides clues to the formation of the Solar system. Particles having formed 4.5 billion years ago can survive planetary accretion and those that survived until now did not evolve significantly since then. Meteoroids and Interplanetary Dust can be observed by measuring the intensity and polarization of the zodiacal light, by observing meteors entering the Earth’s atmosphere, by collecting them in the upper atmosphere, polar ices and snow, and by detecting them with in-situ detectors on space probes.
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Polarization of the Interplanetary Dust Medium (Invited)
2015Co-Authors: Jérémie Lasue, Anny Chantal Levasseur-regourd, Edith HadamcikAbstract:The Interplanetary Dust cloud is visible through its scattered light (the zodiacal light) at visible wavelengths. Brightness observations lead to equilibrium temperature and albedo of the particles and their variation as a function of the heliocentric distance. The light scattered by this optically thin medium is linearly polarized with negative values of the degree of linear polarization, PQ, in the backscattering region. We will review the zodiacal light photopolarimetric observations from the whole line–of-sight integrated values to the local values retrieved by inversion. Whenever available, the local PQ variation as a function of the phase angle presents a phase curve with a small negative branch and large positive branch similar to comets or asteroids. PQ does not seem to show a wavelength variation. The maximum of polarization decreases with decreasing heliocentric distance. A circular polarization signal may be present in parts of the sky. Both numerical simulations and laboratory experiments of light scattering by irregular particles have been performed to constrain the Interplanetary Dust properties based on their polarimetric signature. These studies indicate that mixtures of low-absorption (Mg-silicates) and high-absorption (carbonaceous) particles can explain the intensity and polarimetric observations of the zodiacal cloud. The variations with the heliocentric distance may be due to decreasing carbonaceous content of the Dust cloud. Such models would favor a significant proportion of aggregates and absorbing particles in the Interplanetary Dust medium, indicative of a major cometary Dust contribution. The exact origin (asteroidal, cometary, interstellar) and physical properties of the Dust particles contributing to the zodiacal cloud is still debated and will be more constrained with future observations. New high-resolution systems will monitor the zodiacal light from the ground and new results are expected from upcoming space missions.
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Interplanetary Dust
2015Co-Authors: Jérémie Lasue, Anny Chantal Levasseur-regourd, Alexander LazarianAbstract:This chapter reviews how the polarization of light scattered by Interplanetary Dust has been used to determine some physical properties of the Dust population in the Interplanetary medium. Though optically thin, the Interplanetary Dust cloud is visible due to the faint glow (the zodiacal light) it produces at visible wavelengths through the scattering of light from the Sun by Interplanetary Dust particles (IDPs). The light, scattered by an optically thin medium is linearly polarized, with the E-vector predominantly oscillating perpendicular or parallel to the scattering plane, leading to negative values of the degree of linear polarization, PQ, in the backscattering region. The zodiacal light also has an IR component, due to the thermal emission from the Dust particles, whose characteristics are consistent with the conclusions from the polarimetry. While some results from intensity observations are used for discussion in this chapter, complete reviews of the zodiacal light intensity studies can be found in Leinert et al. (1998) and Levasseur-Regourd et al. (2001). Sections 24.1 and 24.2 summarize the zodiacal light photopolarimetric observations, going from the whole line-of-sight integrated values to the local values retrieved by inversion. Sections 24.3 and 24.4 explain how numerical simulations and laboratory experiments have been carried out to constrain the Interplanetary Dust properties at different locations in the cloud based on their polarimetric signatures.
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Polarimetric Studies of Solar Light Scattered by Interplanetary Dust Particles and the Eye-Sat Project
2014Co-Authors: Anny Chantal Levasseur-regourd, Jérémie LasueAbstract:Studying intensity and linear polarization of the solar light scattered by Interplanetary Dust is of interest for various reasons. This so-called zodiacal light constitutes a faint polarized glow that constitutes a changing foreground for observations of faint extended astronomical sources. Besides, analysis of its polarization provides information on properties of the Dust particles, such as spatial density, morphology and complex refractive index. Previous observations, mostly from the Earth and with a resolution in the 10° range, have been used to infer that the local polarization at 90° phase angle increases with increasing solar distance. Numerical simulations suggest that, in the inner solar system, Interplanetary Dust particles consist of a mixture of absorbing and less absorbing materials, and that radial changes originate in a decrease of organic materials with decreasing solar distance under alteration or evaporation processes. To improve the quality of data on zodiacal light polarimetry, Eye-Sat nanosat is being developed in the context of the JANUS CNES cubesats program for students. The project is now in phase C-D, for a piggy-back launch in 2016. Eye-Sat triple cubesat is anticipated to demonstrate the feasibility of a series of new on-board technologies. Moreover, during its one-year mission, zodiacal light intensity and polarization are to be measured, for the first time with a spatial resolution of about 1° over a wide portion of the sky and in four different wavelengths (visible to near-IR), leading to a better assessment of Interplanetary Dust properties. Finally, a significant fraction of the Interplanetary Dust is estimated to come from comets, the most pristine objects to be found in the inner solar system. While similarities have indeed been noticed between polarimetric properties of Interplanetary and cometary Dust particles, the latter being currently extensively documented by the Rosetta mission to comet 67P/Churyumov-Gerasimenko, further studies of Interplanetary Dust should provide a better insight on possible delivery of carbonaceous particles on telluric planets through Dust impacts at an epoch of heavy bombardment, and thus to the early solar system evolution. Support from CNES is warmly acknowledged.
Jérémie Lasue - One of the best experts on this subject based on the ideXlab platform.
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Interplanetary Dust, Meteoroids, Meteors and Meteorites
Space Science Reviews, 2019Co-Authors: Detlef Koschny, Jérémie Lasue, Anny Chantal Levasseur-regourd, George J. Flynn, Rachel H. Soja, Cecile Engrand, David Malaspina, Tomoki Nakamura, Andrew R. Poppe, Veerle J. SterkenAbstract:Interplanetary Dust particles and meteoroids mostly originate from comets and asteroids. Understanding their distribution in the Solar system, their dynamical behavior and their properties, sheds light on the current state and the dynamical behavior of the Solar system. Dust particles can endanger Earth-orbiting satellites and deep-space probes, and a good understanding of the spatial density and velocity distribution of Dust and meteoroids in the Solar system is important for designing proper spacecraft shielding. The study of Interplanetary Dust and meteoroids provides clues to the formation of the Solar system. Particles having formed 4.5 billion years ago can survive planetary accretion and those that survived until now did not evolve significantly since then. Meteoroids and Interplanetary Dust can be observed by measuring the intensity and polarization of the zodiacal light, by observing meteors entering the Earth’s atmosphere, by collecting them in the upper atmosphere, polar ices and snow, and by detecting them with in-situ detectors on space probes.
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Interplanetary Dust, Meteoroids, Meteors and Meteorites
Space Science Reviews, 2019Co-Authors: Detlef Koschny, Jérémie Lasue, Anny Chantal Levasseur-regourd, George J. Flynn, Rachel H. Soja, Cecile Engrand, David Malaspina, Tomoki Nakamura, Andrew R. Poppe, Veerle J. SterkenAbstract:Interplanetary Dust particles and meteoroids mostly originate from comets and asteroids. Understanding their distribution in the Solar system, their dynamical behavior and their properties, sheds light on the current state and the dynamical behavior of the Solar system. Dust particles can endanger Earth-orbiting satellites and deep-space probes, and a good understanding of the spatial density and velocity distribution of Dust and meteoroids in the Solar system is important for designing proper spacecraft shielding. The study of Interplanetary Dust and meteoroids provides clues to the formation of the Solar system. Particles having formed 4.5 billion years ago can survive planetary accretion and those that survived until now did not evolve significantly since then. Meteoroids and Interplanetary Dust can be observed by measuring the intensity and polarization of the zodiacal light, by observing meteors entering the Earth’s atmosphere, by collecting them in the upper atmosphere, polar ices and snow, and by detecting them with in-situ detectors on space probes.
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Polarization of the Interplanetary Dust Medium (Invited)
2015Co-Authors: Jérémie Lasue, Anny Chantal Levasseur-regourd, Edith HadamcikAbstract:The Interplanetary Dust cloud is visible through its scattered light (the zodiacal light) at visible wavelengths. Brightness observations lead to equilibrium temperature and albedo of the particles and their variation as a function of the heliocentric distance. The light scattered by this optically thin medium is linearly polarized with negative values of the degree of linear polarization, PQ, in the backscattering region. We will review the zodiacal light photopolarimetric observations from the whole line–of-sight integrated values to the local values retrieved by inversion. Whenever available, the local PQ variation as a function of the phase angle presents a phase curve with a small negative branch and large positive branch similar to comets or asteroids. PQ does not seem to show a wavelength variation. The maximum of polarization decreases with decreasing heliocentric distance. A circular polarization signal may be present in parts of the sky. Both numerical simulations and laboratory experiments of light scattering by irregular particles have been performed to constrain the Interplanetary Dust properties based on their polarimetric signature. These studies indicate that mixtures of low-absorption (Mg-silicates) and high-absorption (carbonaceous) particles can explain the intensity and polarimetric observations of the zodiacal cloud. The variations with the heliocentric distance may be due to decreasing carbonaceous content of the Dust cloud. Such models would favor a significant proportion of aggregates and absorbing particles in the Interplanetary Dust medium, indicative of a major cometary Dust contribution. The exact origin (asteroidal, cometary, interstellar) and physical properties of the Dust particles contributing to the zodiacal cloud is still debated and will be more constrained with future observations. New high-resolution systems will monitor the zodiacal light from the ground and new results are expected from upcoming space missions.
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Interplanetary Dust
2015Co-Authors: Jérémie Lasue, Anny Chantal Levasseur-regourd, Alexander LazarianAbstract:This chapter reviews how the polarization of light scattered by Interplanetary Dust has been used to determine some physical properties of the Dust population in the Interplanetary medium. Though optically thin, the Interplanetary Dust cloud is visible due to the faint glow (the zodiacal light) it produces at visible wavelengths through the scattering of light from the Sun by Interplanetary Dust particles (IDPs). The light, scattered by an optically thin medium is linearly polarized, with the E-vector predominantly oscillating perpendicular or parallel to the scattering plane, leading to negative values of the degree of linear polarization, PQ, in the backscattering region. The zodiacal light also has an IR component, due to the thermal emission from the Dust particles, whose characteristics are consistent with the conclusions from the polarimetry. While some results from intensity observations are used for discussion in this chapter, complete reviews of the zodiacal light intensity studies can be found in Leinert et al. (1998) and Levasseur-Regourd et al. (2001). Sections 24.1 and 24.2 summarize the zodiacal light photopolarimetric observations, going from the whole line-of-sight integrated values to the local values retrieved by inversion. Sections 24.3 and 24.4 explain how numerical simulations and laboratory experiments have been carried out to constrain the Interplanetary Dust properties at different locations in the cloud based on their polarimetric signatures.
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Polarimetric Studies of Solar Light Scattered by Interplanetary Dust Particles and the Eye-Sat Project
2014Co-Authors: Anny Chantal Levasseur-regourd, Jérémie LasueAbstract:Studying intensity and linear polarization of the solar light scattered by Interplanetary Dust is of interest for various reasons. This so-called zodiacal light constitutes a faint polarized glow that constitutes a changing foreground for observations of faint extended astronomical sources. Besides, analysis of its polarization provides information on properties of the Dust particles, such as spatial density, morphology and complex refractive index. Previous observations, mostly from the Earth and with a resolution in the 10° range, have been used to infer that the local polarization at 90° phase angle increases with increasing solar distance. Numerical simulations suggest that, in the inner solar system, Interplanetary Dust particles consist of a mixture of absorbing and less absorbing materials, and that radial changes originate in a decrease of organic materials with decreasing solar distance under alteration or evaporation processes. To improve the quality of data on zodiacal light polarimetry, Eye-Sat nanosat is being developed in the context of the JANUS CNES cubesats program for students. The project is now in phase C-D, for a piggy-back launch in 2016. Eye-Sat triple cubesat is anticipated to demonstrate the feasibility of a series of new on-board technologies. Moreover, during its one-year mission, zodiacal light intensity and polarization are to be measured, for the first time with a spatial resolution of about 1° over a wide portion of the sky and in four different wavelengths (visible to near-IR), leading to a better assessment of Interplanetary Dust properties. Finally, a significant fraction of the Interplanetary Dust is estimated to come from comets, the most pristine objects to be found in the inner solar system. While similarities have indeed been noticed between polarimetric properties of Interplanetary and cometary Dust particles, the latter being currently extensively documented by the Rosetta mission to comet 67P/Churyumov-Gerasimenko, further studies of Interplanetary Dust should provide a better insight on possible delivery of carbonaceous particles on telluric planets through Dust impacts at an epoch of heavy bombardment, and thus to the early solar system evolution. Support from CNES is warmly acknowledged.
M. Ishiguro - One of the best experts on this subject based on the ideXlab platform.
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origin of Interplanetary Dust through optical properties of zodiacal light
The Astrophysical Journal, 2015Co-Authors: Hongu Yang, M. IshiguroAbstract:This study investigates the origin of Interplanetary Dust particles (IDPs) through the optical properties, albedo and spectral gradient, of zodiacal light. The optical properties were compared with those of potential parent bodies in the solar system, which include D-type (as analogs of cometary nuclei), C-type, S-type, X-type, and B-type asteroids. We applied Bayesian inference to the mixture model composed of the distribution of these sources, and found that >90% of the IDPs originate from comets (or their spectral analogs, D-type asteroids). Although some classes of asteroids (C-type, X-type, and B-type) may make a moderate contribution, ordinary chondrite-like particles from S-type asteroids occupy a negligible fraction of the Interplanetary Dust cloud complex. The overall optical properties of the zodiacal light were similar to those of chondritic porous IDPs, supporting the dominance of cometary particles in the zodiacal cloud.
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Origin of Interplanetary Dust through Optical Properties of Zodiacal Light
The Astrophysical Journal, 2015Co-Authors: Hongu Yang, M. IshiguroAbstract:This study investigates the origin of Interplanetary Dust particles (IDPs) through the optical properties, albedo and spectral gradient, of zodiacal light. The optical properties were compared with those of potential parent bodies in the solar system, which include D-type (as analogue of cometary nuclei), C-type, S-type, X-type, and B-type asteroids. We applied Bayesian inference on the mixture model made from the distribution of these sources, and found that >90% of the Interplanetary Dust particles originate from comets (or its spectral analogues, D-type asteroids). Although some classes of asteroids (C-type and X-type) may make a moderate contribution, ordinary chondrite-like particles from S-type asteroids occupy a negligible fraction of the Interplanetary Dust cloud complex. The overall optical properties of the zodiacal light were similar to those of chondritic porous IDPs, supporting the dominance of cometary particles in zodiacal cloud.
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Observational Studies of Interplanetary Dust
Small Bodies in Planetary Systems, 2008Co-Authors: M. Ishiguro, M. UenoAbstract:We describe recent developments in observations of Interplanetary Dust particles. These developments are largely due to the introduction of cooled charge coupled device detectors and two-dimensional infrared array detectors with infrared space telescopes. The new observational data show not only the global structure of the Interplanetary Dust cloud, e.g., its symmetric plane, but also the faint structures, such as the asteroidal Dust bands and the cometary Dust trails seen as a brightness enhancement of a few percents above that of the smooth component. Spectrographic observations provide some knowledge about the dynamics and composition of these local components. We mention sources of Interplanetary Dust particles revealed by these observations. In the last chapter, we introduce ongoing and future projects related to the observational study of Interplanetary Dust.
Hongu Yang - One of the best experts on this subject based on the ideXlab platform.
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Origin of Interplanetary Dust through Optical Properties of Zodiacal Light
The Astrophysical Journal, 2015Co-Authors: Hongu Yang, M. IshiguroAbstract:This study investigates the origin of Interplanetary Dust particles (IDPs) through the optical properties, albedo and spectral gradient, of zodiacal light. The optical properties were compared with those of potential parent bodies in the solar system, which include D-type (as analogue of cometary nuclei), C-type, S-type, X-type, and B-type asteroids. We applied Bayesian inference on the mixture model made from the distribution of these sources, and found that >90% of the Interplanetary Dust particles originate from comets (or its spectral analogues, D-type asteroids). Although some classes of asteroids (C-type and X-type) may make a moderate contribution, ordinary chondrite-like particles from S-type asteroids occupy a negligible fraction of the Interplanetary Dust cloud complex. The overall optical properties of the zodiacal light were similar to those of chondritic porous IDPs, supporting the dominance of cometary particles in zodiacal cloud.
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origin of Interplanetary Dust through optical properties of zodiacal light
The Astrophysical Journal, 2015Co-Authors: Hongu Yang, M. IshiguroAbstract:This study investigates the origin of Interplanetary Dust particles (IDPs) through the optical properties, albedo and spectral gradient, of zodiacal light. The optical properties were compared with those of potential parent bodies in the solar system, which include D-type (as analogs of cometary nuclei), C-type, S-type, X-type, and B-type asteroids. We applied Bayesian inference to the mixture model composed of the distribution of these sources, and found that >90% of the IDPs originate from comets (or their spectral analogs, D-type asteroids). Although some classes of asteroids (C-type, X-type, and B-type) may make a moderate contribution, ordinary chondrite-like particles from S-type asteroids occupy a negligible fraction of the Interplanetary Dust cloud complex. The overall optical properties of the zodiacal light were similar to those of chondritic porous IDPs, supporting the dominance of cometary particles in the zodiacal cloud.
