The motion of charged dust particles in interplanetary space—I. The zodiacal dust cloud

1979 ◽  
Vol 27 (10) ◽  
pp. 1269-1282 ◽  
Author(s):  
G.E. Morfill ◽  
E. Grün
Keyword(s):  
Interplanetary Space ◽  
Dust Cloud ◽  
Dust Particles ◽  
Charged Dust ◽  
Zodiacal Dust

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

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

<p align="justify">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/Δm ≈ 100-150), mass, electrical charge, velocity (about 10% accuracy), and impact direction (about 10° accuracy).</p> <p align="justify">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.</p> <p align="justify">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.</p> <p align="justify">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.</p>

scholarly journals The Motion of Charged Dust Particles in Interplanetary Space

1980 ◽  
Vol 90 ◽  
pp. 309-310
Author(s):  
G. E. Morfill ◽  
E. Grün
Keyword(s):  
Magnetic Field ◽  
Current Sheet ◽  
Equatorial Plane ◽  
Particle Motion ◽  
Large Scale ◽  
Interplanetary Space ◽  
Dust Particles ◽  
Charged Dust ◽  
Particle Orbits ◽  
Interplanetary Plasma

The problem of electromagnetic perturbations of charged dust particle orbits in interplanetary space has been re-examined in the light of our better understanding of the large scale spatial and temporal interplanetary plasma and field topology. In the equatorial plane, the magnetic sectors, caused by the warped current sheet, produce stochastic orbit perturbations. From this a diffusive description of particle motion can be derived, provided the dust particles are sufficiently small. The effects of large unipolar magnetic field regions at high heliographic latitudes will be briefly discussed.

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.

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.

Antiprobcotron magnetic trap for charged dust particles in space experiments

2019 ◽  
pp. 20-29
Author(s):  
Lev G. D’YACHKOV ◽  
Mikhail M. VASILYEV ◽  
Oleg F. PETROV ◽  
Sergey F. SAVIN ◽  
Igor V. CHURILO
Keyword(s):  
Magnetic Trap ◽  
Space Station ◽  
Coulomb Systems ◽  
Inhomogeneous Magnetic Field ◽  
Dust Particles ◽  
Charged Dust ◽  
Magnetic Traps ◽  
Space Experiments ◽  
Microgravity Conditions ◽  
New Space

We discuss the possibility of using static magnetic traps as an alternative to electrostatic traps for forming and confining structures of charged dust particles in a gas discharge plasma in the context of our study of strongly interacting Coulomb systems. Some advantages of confining structures in magnetic traps over electrostatic ones are shown. Also we provide a review of the related researches carried out first in laboratory conditions, and then under microgravity conditions including the motivation of performing the experiments aboard the International Space Station (ISS). The preparations of a new space experiment «Coulomb-magnet» as well as the differences of a new equipment from previously used are described. We proposed the main tasks of the new experiment as a study of the dynamics and structure of active monodisperse and polydisperse macroparticles in an inhomogeneous magnetic field under microgravity conditions, including phase transitions and the evolution of such systems in the kinetic heating of dust particles by laser radiation. Key words: Coulomb structures, magnetic trap, antiprobotron, diamagnetic particles, dust particles, microgravity.

scholarly journals A new method of inferring the size, number density, and charge of mesospheric dust from its in situ collection by the DUSTY probe

2019 ◽  
Vol 12 (3) ◽  
pp. 1673-1683 ◽  
Author(s):  
Ove Havnes ◽  
Tarjei Antonsen ◽  
Gerd Baumgarten ◽  
Thomas W. Hartquist ◽  
Alexander Biebricher ◽  
...  
Keyword(s):  
New Method ◽  
Production Model ◽  
Dust Particles ◽  
Bottom Plate ◽  
Charged Dust ◽  
Fundamental Parameters ◽  
Dust Charge ◽  
Analysis Technique ◽  
June July ◽  
The Impact

Abstract. We present a new method of analyzing measurements of mesospheric dust made with DUSTY rocket-borne Faraday cup probes. It can yield the variation in fundamental dust parameters through a mesospheric cloud with an altitude resolution down to 10 cm or less if plasma probes give the plasma density variations with similar height resolution. A DUSTY probe was the first probe that unambiguously detected charged dust and aerosol particles in the Earth's mesosphere. DUSTY excluded the ambient plasma by various biased grids, which however allowed dust particles with radii above a few nanometers to enter, and it measured the flux of charged dust particles. The flux measurements directly yielded the total ambient dust charge density. We extend the analysis of DUSTY data by using the impact currents on its main grid and the bottom plate as before, together with a dust charging model and a secondary charge production model, to allow the determination of fundamental parameters, such as dust radius, charge number, and total dust density. We demonstrate the utility of the new analysis technique by considering observations made with the DUSTY probes during the MAXIDUSTY rocket campaign in June–July 2016 and comparing the results with those of other instruments (lidar and photometer) also used in the campaign. In the present version we have used monodisperse dust size distributions.

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