Zodiacal Dust Particles: Some Comments on Recent Evidence concerning their Motion

Nature ◽  
1969 ◽  
Vol 224 (5214) ◽  
pp. 54-55 ◽  
Author(s):  
N. K. REAY
Keyword(s):  
Dust Particles ◽  
Zodiacal Dust

Optical and Thermal Properties of Zodiacal Dust

1996 ◽  
Vol 150 ◽  
pp. 301-308 ◽  
Author(s):  
A.C. Levasseur-Regourd
Keyword(s):  
Thermal Properties ◽  
Physical Properties ◽  
Bulk Density ◽  
Thermal Emission ◽  
Symmetry Plane ◽  
Dust Particles ◽  
Orbital Inclination ◽  
Zodiacal Dust ◽  
Dust Distribution

AbstractRecent progress has been reported in the determination of the zodiacal thermal emission, brightness and polarization. These results, of interest to estimate the foreground sources in astrophysical observations, do not provide immediately information on the dust distribution, and on its optical and thermal properties. To infer local information about the bulk density, and the physical properties of the dust particles, it is necessary to compare the observations with realistic models or to invert the line-of-sight data. The latter approach typically suggests that the bulk density is (in the symmetry plane) inversely proportional to the solar distance, that the particles are not spheroidal, but rather irregular in shape, that their physical properties change with their distance to the Sun and their orbital inclination, and finally that they do not emit like a blackbody. The heterogeneity noticed in the cloud is due to various sources of dust particles, the size, shape or albedo of which evolve as a function of time, under collision and/or evaporation processes.

scholarly journals A Method for Deriving the Mean Volume Scattering Phase Function for Zodiacal Dust

1985 ◽  
Vol 85 ◽  
pp. 215-218
Author(s):  
S.S. Hong
Keyword(s):  
Linear Combination ◽  
Phase Function ◽  
Dust Particles ◽  
Zodiacal Light ◽  
Volume Scattering ◽  
Zodiacal Dust ◽  
Scattering Phase ◽  
The Mean ◽  
Scattering Phase Function ◽  
Phase Functions

AbstractA linear combination of 3 Henyey-Greenstein phase functions is substituted for the mean volume scattering phase function in the zodiacal light brightness integral. Results of the integral are then compared with the observed brightness to form residuals. Minimization of the residuals provides us with the best combination of Henyey-Greenstein functions for the scattering phase function of zodiacal dust particles.

Model Calculations of the F-Corona and inner Zodiacal Light

2020 ◽  
Author(s):  
Saliha Eren ◽  
Ingrid Mann
Keyword(s):  
Size Distribution ◽  
White Light ◽  
Scattered Light ◽  
Mie Scattering ◽  
Dust Particles ◽  
Line Of Sight ◽  
The Sun ◽  
Zodiacal Light ◽  
Model Calculations ◽  
Zodiacal Dust

<p>The white-light Fraunhofer corona (F-corona) and inner Zodiacal light are generated by interplanetary (Zodiacal) dust particles that are located between Sun and observer. At visible wavelength the brightness comes from sunlight scattered at the dust particles. F-corona and inner Zodiacal light were recently observed from STEREO (Stenborg et al. 2018) and Parker Solar Probe (Howard et al. 2019) spacecraft which motivates our model calculations. We investigate the brightness by integration of scattered light along the line of sight of observations. We include a three-dimensional distribution of the Zodiacal dust that describes well the brightness of the Zodiacal light at larger elongations, a dust size distribution derived from observations at 1AU and assume Mie scattering at silicate particles to describe the scattered light over a large size distribution from 1 nm to 100 µm. From our simulations, we calculate the flattening index of the F-corona, which is the ratio of the minor axis to the major axis found for isophotes at different distances from the Sun, respectively elongations of the line of sight. Our results agree well with results from STEREO/SECCHI observational data where the flattening index varies from 0.45° and 0.65° at elongations between 5° and 24°. To compare with Parker Solar Probe observations, we investigate how the brightness changes when the observer moves closer to the Sun. This brightness change is influenced by the dust number density along the line of sight and by the changing scattering geometry.</p><p>-Stenborg G., Howard R. A., and Stauffer J. R., 2018: Characterization of the White-light Brightness of the F-corona between 5° and 24° Elongation, Astrophys. J. 862: 168 (21pp).</p><p>-Howard, R.A. and 25 co-authors, 2019: Near-Sun observations of an F-corona decrease and K-corona fine structure, Nature 576, 232–236.</p>

scholarly journals Electromagnetic Escape of Dust from the Solar System

1996 ◽  
Vol 150 ◽  
pp. 31-34 ◽  
Author(s):  
Douglas P. Hamilton ◽  
Eberhard Grün ◽  
Michael Baguhl
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Solar System ◽  
Solar Magnetic Field ◽  
Ecliptic Plane ◽  
Dust Particles ◽  
Orbital Dynamics ◽  
Zodiacal Cloud ◽  
Current Configuration ◽  
Zodiacal Dust

AbstractCollisions of asteroids and among Zodiacal cloud particles produce large amounts of submicron-sized debris, much of which is immediately ejected from our solar system by electromagnetic forces. We investigate the trajectories of tiny grains started on circular uninclined orbits within the Zodiacal cloud and find that they reach high ecliptic latitudes during the current configuration of the solar magnetic.field, perhaps accounting for particles detected by the Ulysses spacecraft at latitudes up to 80°. When the solar magnetic field is reversed, particles are more strongly confined to the ecliptic plane and escape the solar system less readily. Both fluxes and spatial densities of sub-micron sized Zodiacal dust particles vary with time through the dependence of orbital dynamics on the 22-year solar cycle.

scholarly journals Electromagnetic Effects on the Zodiacal Dust Cloud

1980 ◽  
Vol 90 ◽  
pp. 311-311 ◽  
Author(s):  
E. Grün ◽  
G. E. Morfill
Keyword(s):  
Equatorial Plane ◽  
Dust Cloud ◽  
Dust Particles ◽  
Rotational Axis ◽  
Zodiacal Light ◽  
Interplanetary Dust Particles ◽  
Electromagnetic Forces ◽  
Solar Cycle Variation ◽  
Zodiacal Dust ◽  
Electromagnetic Effects

Electromagnetic effects on charged zodiacal dust particles were investigated. It can be shown that: 1) stochastic variations induced by electromagnetic forces are unimportant for the zodiacal dust cloud except for the lowest masses, 2) systematic variations in orbit inclinations are unimportant if orbital radii are larger than 10 A.U. This is due to the solar cycle variation in magnetic polarity which tends to cancel out systematic effects, 3) systematic variations in orbital parameters (inclination, longitude of ascending node, longitude of perihelion) induced by electromagnetic forces inside 1 A.U. tend to shift the plane of symmetry of the zodiacal dust cloud somewhat towards the solar magnetic equatorial plane, 4) inside 0.3 A.U. there is a possibility that dust particles may enter a region of “magnetically resonant” orbits for some time. Changes in orbit parameters are then correspondingly enhanced, 5) the observed similarity of the plane of symmetry of zodiacal light with the solar equatorial plane may be the effect of the interaction of charged interplanetary dust particles with the interplanetary magnetic field. Numerical orbit calculation of dust particles show that one of the results of this interaction is the rotation of the orbit plane about the solar rotational axis.

Nonspherical zodiacal dust particles driven by radiation pressure

2010 ◽  
Vol 58 (7-8) ◽  
pp. 1050-1054
Author(s):  
J. Klačka ◽  
M. Kocifaj ◽  
G. Wurm ◽  
P. Wehry ◽  
J. Teiser
Keyword(s):  
Radiation Pressure ◽  
Dust Particles ◽  
Zodiacal Dust

scholarly journals Interplanetary Dust Close to the Sun

1991 ◽  
Vol 126 ◽  
pp. 187-190
Author(s):  
Ingrid Mann
Keyword(s):  
Remote Sensing ◽  
Thermal Emission ◽  
Dust Cloud ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
The Sun ◽  
Zodiacal Dust ◽  
In Situ Experiments ◽  
Infrared Brightness

AbstractThe optical and infrared brightness of the Fraunhofer-corona is produced by light scattering at the zodiacal dust particles and by their thermal emission (see Koutchmy and Lamy 1985). It is modelled within the ecliptic (4 Ro≤ ε ≤ 15 Ro)taking into account investigations of the global zodiacal dust cloud due to remote sensing and in situ experiments. The input of near solar dust to the corona brightness is discussed.

scholarly journals Spatially Varying Optical Properties of the Zodiacal Dust

1989 ◽  
Vol 8 ◽  
pp. 267-272
Author(s):  
S. S. Hong ◽  
S. M. Kwon
Keyword(s):  
Optical Properties ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
The Sun ◽  
Zodiacal Light ◽  
Interplanetary Dust Particles ◽  
Ample Evidence ◽  
Mixing Ratios ◽  
Zodiacal Dust ◽  
Spatially Varying

AbstractAnalyses of both the zodiacal light in the visible and the zodiacal emission in the infrared have provided us with ample evidence to claim that the interplanetary dust particles are mixtures or coagulations of more than one constituents and their mixing ratios vary with the distance from the sun.

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