Asteroidal Dust

Asteroids III ◽  
2002 ◽  
pp. 423-442
Author(s):  
Stanley F. Dermott ◽  
Daniel D. Durda ◽  
Keith Grogan ◽  
Thomas J. J. Kehoe
Keyword(s):  
Asteroidal Dust

scholarly journals Estimating the Asteroidal Component of the Zodiacal Cloud using the Earth's Resonant Ring

1996 ◽  
Vol 150 ◽  
pp. 155-158 ◽  
Author(s):  
Sumita Jayaraman ◽  
Stanley F. Dermott
Keyword(s):  
Surface Area ◽  
Frequency Distribution ◽  
Size Range ◽  
Dust Cloud ◽  
Dust Particles ◽  
Direct Function ◽  
Size Frequency Distribution ◽  
Limited Size ◽  
Zodiacal Cloud ◽  
Asteroidal Dust

AbstractThe Earth's resonant ring is populated primarily by asteroidal dust particles because cometary particles have higher Poynting-Robertson drag rates and the Earth's resonances are not strong enough to trap them (Gomes, 1995). It has been shown that asteroidal particles in a limited size range from 5 — 30μm are responsible for the observed trailing/leading flux asymmetry caused by the trailing dust cloud embedded in the ring (Jayaraman and Dermott 1995). The magnitude of the flux asymmetry is a direct function of the area of dust in the ring, which in turn depends upon the number of asteroidal particles in the zodiacal cloud. Using a dynamical model of the ring and the background zodiacal cloud and estimating the surface area of dust needed in the ring to match the observed flux asymmetry in the 25 micron COBE waveband, we have calculated the fraction of asteroidal dust in the zodiacal cloud as a function of p, the slope of the size-frequency distribution of particles.

scholarly journals The Distribution of Asteroidal Dust in the Inner Solar System

2004 ◽  
Vol 202 ◽  
pp. 184-186
Author(s):  
Keith Grogan ◽  
S.F. Dermott ◽  
T.J.J. Kehoe
Keyword(s):  
Solar System ◽  
Parent Body ◽  
Asteroid Belt ◽  
Dust Particles ◽  
Secular Resonances ◽  
Level Of Confidence ◽  
Asteroidal Dust

In this paper we demonstrate how the action of secular resonances near the inner edge of the asteroid belt strongly effects the inclinations and eccentricities of asteroidal dust particles, such that they lose the orbital characteristics of their parent body and are dispersed into the zodiacal background. As a consequence, it may not be possible to relate the distribution of interplanetary material at 1 AU to given asteroidal or cometary sources with the level of confidence previously imagined.

scholarly journals Dynamics of the Zodiacal Cloud

1992 ◽  
Vol 152 ◽  
pp. 333-347 ◽  
Author(s):  
S. F. Dermott ◽  
R. S. Gomes ◽  
D. D. Durda ◽  
B. Å. S. Gustafson ◽  
S. Jayaraman ◽  
...  
Keyword(s):  
Solar System ◽  
Dust Particle ◽  
Thermal Flux ◽  
Complex Structure ◽  
Dust Cloud ◽  
Three Dimensional ◽  
The Sun ◽  
Particle Orbits ◽  
Analysis Center ◽  
Asteroidal Dust

Advances in infrared astronomy and in computing power have recently opened up an interesting area of the solar system for dynamical exploration. The survey of the sky made by The Infrared Astronomical Satellite (IRAS) in 1983 revealed the complex structure of the zodiacal dust cloud. We now know the inclination and nodes of the plane of symmetry of the cloud with respect to the ecliptic and we have evidence that the cloud is not rotationally symmetric with respect to the Sun. Of even more interest is the discovery by IRAS of prominent dust bands that circle the Sun in planes near-parallel to the ecliptic. In 1984, we suggested (Dermott et al., Nature, 312, 505-509) that the solar system dust bands discovered by IRAS are produced by the gradual comminution of the asteroids in the major Hirayama asteroid families. The confirmation of this hypothesis has involved: (1) The development of a new secular perturbation theory that includes the effects of Poynting-Robertson light drag on the evolution of the dust particle orbits; (2) The production of a new high resolution Zodiacal History File by IPAC (the Infrared Processing and Analysis Center at Caltech); (3) The development of the SIMUL code: a three-dimensional numerical model that allows the calculation of the thermal flux produced by any particular distribution of dust particle orbits. SIMUL includes the effects of planetary perturbations and PR drag on the dust particle orbits and reproduces the exact viewing geometry of the IRAS telescope. We report that these tools allow us to account in detail for the observed structure of the dust bands. They also allow us to show that there is evidence in the IRAS data for the transport of asteroidal dust from the main belt to the Earth by Poynting-Robertson light drag.

scholarly journals SIRTF: A Unique Opportunity for Probing the Zodiacal Cloud

1996 ◽  
Vol 150 ◽  
pp. 159-162
Author(s):  
Sumita Jayaraman ◽  
Stanley F. Dermott ◽  
Michael Werner
Keyword(s):  
Thermal Emission ◽  
Dust Cloud ◽  
Thermal Characteristics ◽  
Dust Particles ◽  
Infrared Telescope ◽  
The Earth ◽  
Telescope Facility ◽  
Asteroidal Dust ◽  
Infrared Telescope Facility ◽  
Dust Ring

AbstractThe Space Infrared Telescope Facility (SIRTF) is planned for launch by NASA in 2001 in a heliocentric orbit at 1.01 AU The spacecraft will drift away from the Earth slowly, reaching a distance of 0.3 AU behind the Earth at the end of its 2.5 year mission. This implies that SIRTF will spiral through the Earth's resonant dust ring (Wright et al., 1995) and, in particular, that it will traverse the dust cloud in the ring that trails the Earth in its orbit. We have used a dynamical model of the ring (Dermott et al., 1994) followed by simulation of the SIRTF orbit to predict the variations in the zodiacal thermal emission due to the trailing dust cloud as seen by SIRTF. Because the dust ring is inclined to the ecliptic, the latitude of peak flux of the trailing cloud will have yearly oscillations about the ecliptic. The amplitude of the oscillations will increase as SIRTF approaches the cloud, reaching a maximum of 20 during the mission. The magnitude of the flux variations can be as high as 4 – 5% or 2–3 MJy/Sr, SIRTF's measurements of these effects will allow us to model the number density and thermal characteristics of asteroidal dust particles near the Earth.

scholarly journals Asteroidal Dust and the Zodiacal Emission

1991 ◽  
Vol 126 ◽  
pp. 211-214
Author(s):  
William T. Reach
Keyword(s):  
Asteroid Belt ◽  
Color Temperature ◽  
Infrared Background ◽  
Asteroidal Dust ◽  
Band Pair ◽  
Asteroid Families

AbstractThe contribution to the brightness of the infrared background by asteroidal dust, distinguished both by lower color temperature and ‘band-pair’ morphology, is determined using IRAS observations. Dust band pairs are associated with at least 7 asteroid families and groups, but very little is detected from the remainder of the asteroid belt, indicating that asteroid families and groups are the source of asteroidal dust.

The influence of the brightness of the asteroidal dust bands on the gegenschein

Icarus ◽  
2003 ◽  
Vol 162 (2) ◽  
pp. 337-343 ◽  
Author(s):  
T Mukai
Keyword(s):  
Asteroidal Dust

An Asteroidal Dust Ring of Micron-Sized Particles Trapped in the 1:1 Mean Motion Resonance with Jupiter

Icarus ◽  
1995 ◽  
Vol 113 (2) ◽  
pp. 403-414 ◽  
Author(s):  
Jer-Chyi Liou ◽  
Herbert A. Zook
Keyword(s):  
Mean Motion ◽  
Asteroidal Dust ◽  
Dust Ring ◽  
Mean Motion Resonance

scholarly journals IMEM2: a meteoroid environment model for the inner solar system

2019 ◽  
Vol 628 ◽  
pp. A109 ◽  
Author(s):  
R. H. Soja ◽  
E. Grün ◽  
P. Strub ◽  
M. Sommer ◽  
M. Millinger ◽  
...  
Keyword(s):  
Solar System ◽  
Assessment Tool ◽  
Dust Cloud ◽  
Interplanetary Dust ◽  
Diameter Distribution ◽  
Model Parameters ◽  
The Earth ◽  
Source Populations ◽  
Asteroidal Dust ◽  
Dust Complex

Context. The interplanetary dust complex is currently understood to be largely the result of dust production from Jupiter-family comets, with contributions also from longer-period comets (Halley- and Oort-type) and collisionally produced asteroidal dust. Aims. Here we develop a dynamical model of the interplanetary dust cloud from these source populations in order to develop a risk and hazard assessment tool for interplanetary meteoroids in the inner solar system. Methods. The long-duration (1 Myr) integrations of dust grains from Jupiter-family and Halley-type comets and main belt asteroids were used to generate simulated distributions that were compared to COBE infrared data, meteor data, and the diameter distribution of lunar microcraters. This allowed the constraint of various model parameters. Results. We present here the first attempt at generating a model that can simultaneously describe these sets of observations. Extended collisional lifetimes are found to be necessary for larger (radius ≥ 150 μm) particles. The observations are best fit with a differential size distribution that is steep (slope = 5) for radii ≥ 150 μm, and shallower (slope = 2) for smaller particles. At the Earth the model results in ~ 90–98% Jupiter-family comet meteoroids, and small contributions from asteroidal and Halley-type comet particles. In COBE data we find an approximately 80% contribution from Jupiter-family comet meteoroids and 20% from asteroidal particles. The resulting flux at the Earth is mostly within a factor of about two to three of published measurements.

Size Distributions of Asteroidal Dust: Possible Constraints on Impact Strengths

1996 ◽  
Vol 150 ◽  
pp. 473-476
Author(s):  
Daniel D. Durda ◽  
Stanley F. Dermott
Keyword(s):  
Size Distribution ◽  
Size Distributions ◽  
Scaling Properties ◽  
Equilibrium Size ◽  
Asteroidal Dust ◽  
The Impact ◽  
Impact Experiments ◽  
Asteroid Families

AbstractWe present results of a numerical collisional model which shows that the slope index of the equilibrium size distribution is dependent upon the size-strength scaling properties of the colliding bodies. This implies that individual asteroid families or distinct taxonomic classes within the mainbelt asteroid population may evolve different equilibrium size distributions. Well constrained observations of the size distribution over particular size ranges may allow constraints to be placed on the impact strengths of particles much larger or smaller than are capable of being measured in laboratory impact experiments.

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