The influence of the dust-free zone on F-corona brightness

2021 ◽  
Author(s):  
Saliha Eren ◽  
Ingrid Mann
Keyword(s):  
Size Distribution ◽  
Interplanetary Dust ◽  
Spherical Particles ◽  
Dust Particles ◽  
Zodiacal Light ◽  
Forthcoming Article ◽  
Model Calculations ◽  
Free Zone ◽  
Dust Size Distribution ◽  
Density Depletion

<p>This presentation is related to model calculations of the circumsolar dust brightness that is seen in the F-corona and inner Zodiacal light. We calculate the brightness integral that includes the size distribution of the interplanetary dust, the spatial distribution, and the scattering properties. The scattering properties are estimated with Mie calculations of spherical particles consisting of astronomical silicate. We consider different size distributions of the dust particles with sizes between 1 nanometre - 100 micrometre. It was recently discussed that the extension of the dust-free zone can be inferred from the slope of the F-corona brightness seen in new observations received from the WISPR instrument on the NASA Parker Solar Probe (Stenborg et al., 2020). We, therefore, investigate the influence of the dust-free zone on the brightness and compare it to the influence that the dust size distribution has.</p><p>References</p><p>1. G. Stenborg, R. A. Howard, P. Hess, B. Gallagher, PSP/WISPR observations of dust density depletion near the Sun I. Remote observations to 8 Rsol from an observer between 0.13-0.35 AU, A&A, Forthcoming article, 2020. DOI: 10.1051/0004-6361/202039284</p>

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 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.

Effect of an Arbitrary Dust Size Distribution Dust Particles for Vortex-Like Ion Distribution Dusty Plasma

2009 ◽  
Vol 52 (3) ◽  
pp. 517-522
Author(s):  
Wei Ju-Na ◽  
Shi Yu-Ren ◽  
He Guang-Jun ◽  
Jiang Xin ◽  
Duan Wen-Shan ◽  
...  
Keyword(s):  
Size Distribution ◽  
Dusty Plasma ◽  
Dust Particles ◽  
Ion Distribution ◽  
Dust Size Distribution

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 21. Light of the Night Sky / Lumière du Ciel Nocturne

1997 ◽  
Vol 23 (1) ◽  
pp. 231-236
Author(s):  
Christoph Leinert
Keyword(s):  
Interstellar Dust ◽  
Thermal Emission ◽  
Scattered Light ◽  
Diffuse Radiation ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Zodiacal Light ◽  
Interplanetary Dust Particles ◽  
Extragalactic Background Light ◽  
Night Sky

The light of the night sky is a difficult to disentangle mixture of tropospherically scattered light, airglow, zodiacal light (including the thermal emission by interplanetary dust particles), unresolved stellar light, diffuse scattering and emission by interstellar dust and gas, and finally an extragalactic component. It has the reputation of being a very traditional field of astronomy, which certainly is true if we look at the long history of the subject. The recent renewed interest in this topic, which continued during this triennium, appears mainly to come from three sources: - first from the impressive results of the IRAS and COBE infrared satellites. They brought to general consciousness the fact that the infrared sky is characterised by strong emission from interplanetary and interstellar dust, and made clear that this emission may interfere with the study of faint interesting sources. - then from the development of sensitive detectors and arrays for essentially all of the wavelength range to be covered in this report, from the Lyman limit to ≈ 300 μm. Now the difficult measurements of the ultraviolet diffuse radiation and of the extragalactic background light in the infrared cosmological windows around 3 μm and 200 μm have become feasible and state of the art projects. - finally, the threat to astronomical observations arising from man-made development and lighting has become important enough to further studies of uncontaminated and contaminated night sky brightnesses. This report will refer mainly to those areas and is meant to highlight noteworthy developments. It was prepared with the help of Drs. Bowyer and Mattila.

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.

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.

scholarly journals The Motion of Interplanetary Dust Particles

1985 ◽  
Vol 85 ◽  
pp. 81-84
Author(s):  
I.R. East ◽  
N.K. Reay
Keyword(s):  
Radial Velocity ◽  
Ecliptic Plane ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Light Spectrum ◽  
Zodiacal Light ◽  
Interplanetary Dust Particles ◽  
Radial Velocity Curve ◽  
Fabry Perot ◽  
Hyperbolic Trajectories

AbstractRadial velocity measurements on the solar MgI 5183.618Å Fraunhofer absorption line in the Zodiacal Light spectrum have been made with a microprocessor-controlled servo-stabilised Fabry-Perot interferometer. Observations were made at 5 and 10 degree intervals in the ecliptic plane between morning and evening elongations of 25 degrees. These new data are of much greater precision and coverage than any previously obtained. Obtained over a two year period, the observations show a consistent evening/morning asymmetry in the radial velocity curve with the Gegenschein receding from the Earth at 4 Km/sec. These data do not support the hypothesis that the majority of interplanetary dust grains are in hyperbolic trajectories.

scholarly journals Orbits of Interplanetary Dust Particles Inside 1 AU as Observed by Helios

1985 ◽  
Vol 85 ◽  
pp. 105-111
Author(s):  
E. Grün ◽  
H. Fechtig ◽  
J. Kissel
Keyword(s):  
Probability Distributions ◽  
High Energy ◽  
Interplanetary Dust ◽  
Density Variation ◽  
Dust Particles ◽  
Spatial Density ◽  
Zodiacal Light ◽  
Interplanetary Dust Particles ◽  
Impact Speed ◽  
Flight Direction

AbstractThe in situ dust detectors on board the Helios spaceprobes detected impacts of micrometeoroids between 0.3 AU and 1 AU distance from the sun. Among the measured quantities were mass, impact speed and flight direction of the dust particles. Radial variations of the flux, azimuthal distribution and impact speed are discussed. Significantly different results were obtained for the “apex” particles observed by both ecliptic and south sensors and for the “eccentric” particles detected only by the south sensor. The radial spatial density variation of the “eccentric” particles is compatible with that derived for zodiacal light particles. Whereas the spatial density of “apex” particles peaks at 0.5 to 0.6 AU. From the measured quantities probability distributions of orbital elements were derived for the observed micrometeoroids. About 60% of the observed micrometeoroids (“apex” particles) are on low energy orbits (a ≲ 0.6 AU). About 30% of the particles (“eccentric” particles) had high energy orbits (a ≳ 0.9 AU). More than 10% of the observed particles show high probabilities for travelling on hyperbolic orbits.

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