ORIGIN OF THE INTERPLANETARY DUST CLOUD AROUND THE EARTH

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.

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Origins and Spatial Distribution of Non-Pure Sulfate Particles (NSPs) in the Stratosphere Detected by the Balloon-Borne Light Optical Aerosols Counter (LOAC)

Atmosphere ◽

10.3390/atmos11101031 ◽

2020 ◽

Vol 11 (10) ◽

pp. 1031

Author(s):

Jean-Baptiste Renard ◽

Gwenaël Berthet ◽

Anny-Chantal Levasseur-Regourd ◽

Sergey Beresnev ◽

Alain Miffre ◽

...

Keyword(s):

Spatial Distribution ◽

Sulfuric Acid ◽

Dust Cloud ◽

Volcanic Eruptions ◽

Interplanetary Dust ◽

Meteor Shower ◽

The Earth ◽

Large Particles ◽

Main Component ◽

Aerosol Counter

While water and sulfuric acid droplets are the main component of stratospheric aerosols, measurements performed for about 30 years have shown that non-sulfate particles (NSPs) are also present. Such particles, released from the Earth mainly through volcanic eruptions, pollution or biomass burning, or coming from space, present a wide variety of compositions, sizes, and shapes. To better understand the origin of NSPs, we have performed measurements with the Light Optical Aerosol Counter (LOAC) during 151 flights under weather balloons in the 2013–2019 period reaching altitudes up to 35 km. Coupled with previous counting measurements conducted over the 2004–2011 period, the LOAC measurements indicate the presence of stratospheric layers of enhanced concentrations associated with NSPs, with a bimodal vertical repartition ranging between 17 and 30 km altitude. Such enhancements are not correlated with permanent meteor shower events. They may be linked to dynamical and photophoretic effects lifting and sustaining particles coming from the Earth. Besides, large particles, up to several tens of μm, were detected and present decreasing concentrations with increasing altitudes. All these particles can originate from Earth but also from meteoroid disintegrations and from the interplanetary dust cloud and comets.

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A likely detection of a local interplanetary dust cloud passing near the Earth in the AKARI mid-infrared all-sky map

Astronomy and Astrophysics ◽

10.1051/0004-6361/201628954 ◽

2017 ◽

Vol 603 ◽

pp. A82

Author(s):

D. Ishihara ◽

T. Kondo ◽

H. Kaneda ◽

T. Suzuki ◽

K. Nakamichi ◽

...

Keyword(s):

Dust Cloud ◽

Interplanetary Dust ◽

Mid Infrared ◽

The Earth

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Photometric Axis Measurements of the Zodiacal Light at Large Elongations

Symposium - International Astronomical Union ◽

10.1017/s0074180900066456 ◽

1980 ◽

Vol 90 ◽

pp. 45-48

Author(s):

H. Tanabe ◽

A. Takechi ◽

A. Miyashita

Keyword(s):

Spatial Distribution ◽

Interplanetary Dust ◽

The Sun ◽

Zodiacal Light ◽

The Earth ◽

Photoelectric Measurements ◽

Ecliptic Longitude

Measurement of the position of the photometric axis of the zodiacal light at large elongations (90 ° < λ − λ⊙ < 270°; λ:ecliptic longitude, λ⊙: ecliptic longitude of the sun) provides information about the spatial distribution of the interplanetary dust outside the orbit of the Earth. However, modern photoelectric measurements in this part are scarce, except for the Gegenschein region, because of the observational difficulty due to faintness of this part of the zodiacal light.

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Interferometric Observation of the F-Corona Radial Velocities Field Between 3 and 7 R⊚

International Astronomical Union Colloquium ◽

10.1017/s0252921100084372 ◽

1985 ◽

Vol 85 ◽

pp. 77-80

Author(s):

P.V. Shcheglov ◽

L.I. Shestakova ◽

A.K. Ajmanov

Keyword(s):

Scattered Light ◽

Interplanetary Dust ◽

Radial Velocities ◽

The Sun ◽

Continuous Component ◽

The North ◽

The Earth ◽

Fabry Perot ◽

Interferometric Observation ◽

Sky Brightness

AbstractDuring the July 31, 1981 solar eclipse, F-corona interferograms near MgI λ 5184 Å were obtained using a Fabry-Perot etalon (FPE) with an FWHM of 0.5 Å (corresponding to 30 km/sec) and an image tube. Radial velocities Vr of the interplanetary dust (i.d.) were measured in different directions.Both prograde and retrograde motions of i.d. in the ecliptic region is discovered. Most of velocity values do not exceed 50 km/sec. A negative velocity component appears after averaging all Vr for all directions. Its average increases to − 20 km/sec toward the Sun. Some ejections are observed. The strongest (+ 130 km/sec) is located at the north ecliptic pole at a distance of 6 to 7 R⊙.From the lack of unshifted Fraunhofer lines in the scattered sky light, we conclude that the sky brightness continuous component is predominant and its source is K-corona scattered light in the Earth’ s atmosphere.

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Poynting-Robertson Effect and Collisions in the Interplanetary Dust Cloud

Symposium - International Astronomical Union ◽

10.1017/s0074180900066924 ◽

1980 ◽

Vol 90 ◽

pp. 299-302

Author(s):

Jan Trulsen ◽

Arild Wikan

Keyword(s):

Simulation Model ◽

Dust Cloud ◽

Dynamical Evolution ◽

Interplanetary Dust ◽

Collision Time ◽

The Mean ◽

The Individual ◽

Individual Grains

A simulation model has been developed to study the results of the Poynting-Robertson (PR) effect and collisions on the dynamical evolution of an interplanetary dust cloud. Fragmentational and accretional effects are neglected. With a mean free collision time of the order of the PR lifetime collisional effects become of importance. As the individual grains still spiral inwards collisions act to make the mean eccentricity and inclination of the grain orbits both decrease at comparable rates, giving rise to an expanding fan shaped dust cloud.

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31. The interplanetary dust cloud (survey paper)

Symposium - International Astronomical Union ◽

10.1017/s0074180900019884 ◽

1968 ◽

Vol 33 ◽

pp. 323-342 ◽

Cited By ~ 1

Author(s):

T. R. Kaiser

Keyword(s):

Experimental Data ◽

Present State ◽

Interplanetary Space ◽

Dust Cloud ◽

Interplanetary Dust ◽

Cosmic Dust ◽

Magnitude Distribution ◽

Meteor Streams ◽

Survey Paper ◽

Observational Techniques

The first part of the paper reviews the present state of knowledge of the characteristics of cosmic dust in interplanetary space. Since this is derived from a variety of observational techniques, some attempt is made critically to assess the difficulties in interpretation, particularly those due to differences in observational selection. Attention is drawn to the doubts that recently have arisen concerning the existence of a terrestrial dust cloud. The second part describes some radio investigations of the structure of meteor streams and of the sporadic background. Systematic variations in magnitude distribution with solar longitude which are observed in both the Geminids and Perseids cannot be simply interpreted as due to selective perturbation of the smaller meteoroids. Experimental data are described which point to the existence of considerable radiant structure in the sporadic background.

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Interaction of Lunar Ejecta and the Magnetosphere of the Earth

Symposium - International Astronomical Union ◽

10.1017/s0074180900067176 ◽

1980 ◽

Vol 90 ◽

pp. 425-428

Author(s):

W. M. Alexander ◽

J. D. Corbin

Keyword(s):

Initial Study ◽

Interplanetary Dust ◽

Dust Particles ◽

Interplanetary Dust Particles ◽

Lunar Phases ◽

Gravitational Forces ◽

The Earth ◽

Significant Flux

A significant flux of ejecta from lunar impacts of interplanetary dust particles leaves selenocentric space and enters the magnetosphere of the earth. During favorable lunar phases, 80% of the ejecta enter the magnetosphere where their orbits are determined by electrodynamic as well as gravitational forces. Initial study of the orbital characteristics and perturbations of these magnetosphere ejecta is presented and its implications are discussed.

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Destiny+ Dust Analyzer – Campaign & timeline preparation for interplanetary & interstellar dust observation during the 4-year transfer phase from Earth to Phaethon

10.5194/epsc2020-342 ◽

2020 ◽

Author(s):

Maximilian Sommer ◽

Harald Krüger ◽

Ralf Srama ◽

Takayuki Hirai ◽

Masanori Kobayashi ◽

...

Keyword(s):

Electric Propulsion ◽

Interstellar Dust ◽

Impact Ionization ◽

Interplanetary Space ◽

Dust Cloud ◽

Dust Particles ◽

Transfer Phase ◽

Moon System ◽

The Earth ◽

The Impact

The Destiny+ mission (Demonstration and Experiment of Space Technology for Interplanetary voyage Phaethon fLyby and dUst Science) has been selected as part of its M-class Space Science Program by the Japanese space agency JAXA/ISAS and is set to launch in 2023/2024. The mission target is the active asteroid (3200) Phaethon with a projected flyby in early 2028. The scientific payload consists of two cameras (the Telescopic Camera for Phaethon, TCAP, and the Multi-band Camera for Phaethon, MCAP), and the Destiny+ Dust Analyzer (DDA). DDA is the technological successor to the Cosmic Dust Analyzer (CDA) aboard Cassini-Huygens, which prominently investigated the dust environment of the Saturnian system. The DDA sensor is designed as a combination of impact ionization time-of-flight mass spectrometer and trajectory sensor, which will allow for the analysis of sub-micron and micron sized dust particles with respect to their composition (mass resolution m/&#916;m &#8776; 100-150), mass, electrical charge, velocity (about 10% accuracy), and impact direction (about 10&#176; accuracy). Besides attempting to sample the impact-generated dust cloud around Phaethon during the flyby, DDA will be actively observing the interplanetary & interstellar dust environment over the roughly four years spanning cruise phase from the Earth-Moon system through interplanetary space. After launch into a GTO-like orbit, Destiny+ will first employ its solar-electric propulsion system to spiral up to the lunar orbit within about 18 months, followed by a series of lunar swingbys and interim coasting phases in distant cislunar space, accumulating momentum to leave the Earth-Moon system at high excess velocity. The subsequent roughly 2-year interplanetary transfer to intercept Phaethon will be characterized by moderate orbital eccentricity of up to 0.1 and largely unpowered coasting phases. During these four years, the DDA sensor will benefit from a maximum pointing coverage range enabled by its dual-axis pointing mechanism and spacecraft attitude flexibility (during times of unpowered flight). This will allow for exhaustive mapping and analysis of the different interplanetary dust populations, as well as interstellar dust encountered in the region between 0.9-1.1 AU. Here, we give a progress report on the science planning efforts for the 4-year transfer phase. We present a tentative observation timeline that assigns scientific campaigns to different phases of the mission, taking into account results of various dust models, as well as operational and technical constraints.

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