The Interplanetary Dust Complex and Comets

Comets II ◽  
2004 ◽  
pp. 677-694
Author(s):  
Mark V. Sykes ◽  
Eberhard Grün ◽  
William T. Reach ◽  
Peter Jenniskens
Keyword(s):  
Interplanetary Dust ◽  
Dust Complex

scholarly journals The influx rate of long-period comets in the Earth's neighborhood and their debris contribution to the interplanetary medium

2012 ◽  
Vol 10 (H16) ◽  
pp. 140-140
Author(s):  
Julio Angel Fernández
Keyword(s):  
Steady State ◽  
Interplanetary Medium ◽  
Interplanetary Dust ◽  
Large Contribution ◽  
Influx Rate ◽  
Long Period ◽  
Impact Rate ◽  
Total Magnitude ◽  
Dust Complex ◽  
The Impact

AbstractWe analyze the flux of new and evolved long-period comets (LPCs) reaching the Earth's neighborhood (perihelion distances q < 1.3 AU), their physical lifetimes, and their implications as regards to the amount of meteoritic matter that is being deposited in the near-Earth region. The flux of LPCs with q < 1.3 au is found to be of about 340 ± 40, brighter than absolute total magnitude 8.6 (radius R ~ 0.6 km) (Fernández and Sosa 2012). Bearing in mind that most of these comets disintegrate into meteoritic matter, this represents a large contribution to the interplanetary dust complex which requires an amount of matter of about 10 tons s−1 to keep it in steady state. These aspects, as well as the impact rate with Earth of meteoroids of LPC origin, will be discussed in this presentation.

scholarly journals Sources of Interplanetary Dust

1980 ◽  
Vol 90 ◽  
pp. 211-222 ◽  
Author(s):  
Ľubor Kresák
Keyword(s):  
Equilibrium Problem ◽  
Interplanetary Dust ◽  
Point Of View ◽  
Dust Production ◽  
Cometary Nuclei ◽  
Dissipative Processes ◽  
Potential Sources ◽  
Pass Through ◽  
Dust Complex

It is generally assumed that ejections from active cometary nuclei are the major source of replenishment of the interplanetary dust complex. Conjectures against this concept are usually based on comparison of the quantitative efficiency of the dust production by comets with the efficiency of all the dissipative processes involved. The present paper discusses this problem from the dynamical point of view, tracing the evolution of swarms of cometary ejecta as they pass through different evolutionary stages. It is concluded that the contribution of the present population of active comets, of all revolution periods, is not only inadequate to explain the abundance of interplanetary particles, but also inconsistent with the distribution of their orbits. Other potential sources and their implications for the equilibrium problem are reviewed.

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.

scholarly journals Zodiacal Light and Interplanetary Dust

1985 ◽  
Vol 85 ◽  
pp. 1-6 ◽  
Author(s):  
J.L. Weinberg
Keyword(s):  
Interplanetary Dust ◽  
Zodiacal Light ◽  
Dust Complex

AbstractRecent results on zodiacal light are used to show that optics, dynamics, and infrared must be considered together to properly and fully characterize the interplanetary dust complex.

scholarly journals The Effect of Radiation Pressure on the Restricted Three-body Problem

1980 ◽  
Vol 90 ◽  
pp. 285-288
Author(s):  
Donald W. Schuerman
Keyword(s):  
Radiation Pressure ◽  
Body Problem ◽  
Interplanetary Dust ◽  
Restricted Three Body Problem ◽  
Three Body Problem ◽  
Zodiacal Light ◽  
Gravitational Forces ◽  
Dust Complex ◽  
Three Body ◽  
Space Colonization

The classical restricted three-body problem is generalized to include the force of radiation pressure and the Poynting-Robertson effect. The positions of the Lagrangian points L4 and L5 are found as functions of β, the ratio of radiational to gravitational forces. The Poynting-Robertson effect renders the L4 and L5 points unstable on a time scale (T) long compared to the period of rotation of the two massive bodies. For the solar system, T is given by T = [(1-β)2/3/β] 544 a2 yr where a is the separation between the Sun and the planet in AU. Implications for space colonization and a mechanism for producing asymmetries in the interplanetary dust complex are discussed; testing the latter may be possible from the Zodiacal Light/Background Starlight Experiment aboard the International Solar Polar Mission spacecraft to be launched in 1983.

scholarly journals Cometary and Asteroidal Sources of Interplanetary Dust

1991 ◽  
Vol 126 ◽  
pp. 389-396 ◽  
Author(s):  
Mark V. Sykes
Keyword(s):  
Spatial Resolution ◽  
High Spatial Resolution ◽  
Interplanetary Dust ◽  
Zodiacal Cloud ◽  
Cometary Dust ◽  
Infrared Astronomical Satellite ◽  
Dust Complex ◽  
Astronomical Satellite ◽  
Asteroids And Comets

AbstractThe Infrared Astronomical Satellite has provided extensive observations of the zodiacal cloud at high spatial resolution which will not be matched in the forseeable future. Within the zodiacal cloud, IRAS discovered extended dust structures providing the link between the interplanetary dust complex and the asteroids and comets which are its source. These are the asteroid dust bands and the cometary dust trails.

The IRAS dust band contribution to the interplanetary dust complex - Evidence seen at 60 and 100 microns

1992 ◽  
Vol 104 ◽  
pp. 2236 ◽  
Author(s):  
Stanley G. Love ◽  
Donald E. Brownlee
Keyword(s):  
Interplanetary Dust ◽  
Dust Complex

IDENTIFICATION AND ANALYSIS OF INTERPLANETARY DUST PARTICLES FILTERED FROM ANTARCTIC AIR

2018 ◽  
Author(s):  
Katherine Burgess ◽  
◽  
David Bour ◽  
Rhonda M. Stroud ◽  
Anais Bardyn ◽  
...  
Keyword(s):  
Interplanetary Dust ◽  
Dust Particles ◽  
Interplanetary Dust Particles

Exploring the Solar System

2018 ◽  
Author(s):  
Karel Schrijver
Keyword(s):  
Solar System ◽  
Planetary Systems ◽  
Interplanetary Dust ◽  
Terrestrial Planets ◽  
The Moon ◽  
System P ◽  
Asteroids And Comets

In this chapter, the author summarizes the properties of the Solar System, and how these were uncovered. Over centuries, the arrangement and properties of the Solar System were determined. The distinctions between the terrestrial planets, the gas and ice giants, and their various moons are discussed. Whereas humans have walked only on the Moon, probes have visited all the planets and several moons, asteroids, and comets; samples have been returned to Earth only from our moon, a comet, and from interplanetary dust. For Earth and Moon, seismographs probed their interior, whereas for other planets insights come from spacecraft and meteorites. We learned that elements separated between planet cores and mantels because larger bodies in the Solar System were once liquid, and many still are. How water ended up where it is presents a complex puzzle. Will the characteristics of our Solar System hold true for planetary systems in general?

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