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Characteristics of charged dust inferred from the Cassini RPWS measurements in the vicinity of Enceladus
Max-Planck-Institute für extraterrestriche Physik, Germany.
KTH, School of Electrical Engineering (EES), Space and Plasma Physics.ORCID iD: 0000-0002-6712-3625
KTH, School of Electrical Engineering (EES). KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
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2009 (English)In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 57, no 14-15, 1807-1812 p.Article in journal (Refereed) Published
Abstract [en]

The data obtained by the Cassini Radio and Plasma Wave Science (RPWS) instrument during the shallow (17.02.2005) and the steep (14.07.2005) crossings of the E-ring revealed a considerable electron depletion in proximity to Enceladus's orbit (the difference between the ion and electron densities can reach similar to 70 cm(-3)). Assuming that this depletion is a signature of the presence of charged dust particles, the main characteristics of dust down to submicron sized particles are derived. The differential size distribution is found to be well described by a power law with an index mu similar to 5.5-6 for the lower size limit a(min) = 0.03 mu m and mu similar to 7.3-8 for a(min) = 0.1 mu m. The calculated average integral dust number density is weakly affected by values of mu and a(min). For a greater than or similar to 0.1 mu m, both flybys gave the maximum dust density about 0.1-0.3 cm(-3) in the vicinity of Enceladus. Our results imply that the dust structure near Enceladus is characterized by approximately the same vertical length scale of 8000 km and reaches a maximum at the same radial distance (displaced outward of the orbit of Enceladus) as found by Kempf et al. [2008. The E-ring in the vicinity of Enceladus. Spatial distribution and properties of the ring particles. Icarus 193, 420-437], from the dust impact data.

Place, publisher, year, edition, pages
2009. Vol. 57, no 14-15, 1807-1812 p.
Keyword [en]
Saturn moons, E-ring, Cassini, Dust size distribution, Dusty plasma, e-ring, solar-system, plasma, saturn, particles, august
National Category
Fusion, Plasma and Space Physics
Identifiers
URN: urn:nbn:se:kth:diva-12938DOI: 10.1016/j.pss.2009.03.002ISI: 000273099100017Scopus ID: 2-s2.0-70450222133OAI: oai:DiVA.org:kth-12938DiVA: diva2:319765
Note
QC 20100519Available from: 2010-05-19 Created: 2010-05-19 Last updated: 2017-12-12Bibliographically approved
In thesis
1. Object-plasma interaction in the vicinity of Enceladus
Open this publication in new window or tab >>Object-plasma interaction in the vicinity of Enceladus
2010 (English)Licentiate thesis, comprehensive summary (Other academic)
Abstract [en]

    The Cassini spacecraft orbits Saturn since 2004, carrying a multitude of instruments for studies of the plasma environment around the planet as well as the constituents of the ring system. Of particular interest to the present thesis is the large E ring, which consists mainly of water ice grains, smaller than a few micrometres, referred to as dust. The work presented here is concerned with the interaction between, on the one hand, the plasma and, on the other hand, the dust, the spacecraft and the Langmuir probe carried by it. In Paper I, dust densities along the trajectory of Cassini, as it passes through the ring, are inferred from measured electron and ion densities. In Paper II, the situation where a Langmuir probe is located in the potential well of a spacecraft is considered. The importance of knowing the potential structure around the spacecraft and probe is emphasised and its effect on the probe’s current-voltage characteristic is illustrated with a simple analytical model. In Paper III, particle-in-cell simulations are employed to study the potential and density profiles around the Cassini as it travels through the plasma at the orbit of the moon Enceladus.

Abstract [sv]

   Rymdsonden Cassini befinner sig i omloppsbana kring Saturnus sedan 2004 och bär med sig en mångfald av instrument för att studera plasmat och ringarna som omger planeten. Av särskilt intresse i denna licentiatuppsats är den stora E-ringen. Denna utgörs huvudsakligen av mikrometerstora (eller mindre) dammpartiklar, bestående av is. Det arbete som presenteras här behandlar interaktion mellan, å ena sidan, plasmat och, å andra sidan, dammet, rymdsonden och Langmuirprob som denna är utrustad med. I den bilagda Paper I utvinns dammtätheter längs Cassinis bana genom E-ringen ur mätta elektron- och jontätheter. I Paper II betraktas situationen där en Langmuirprob befinner sig i potentialgropen som omger en rymdsond. Här betonas vikten av att ta hänsyn till potentialstrukturen kring rymdsond och prob, och en enkel analytisk modell används för att illustrera hur probens ström-spänningskaraktäristik kan påverkas av denna potentialstruktur. I Paper III studeras täthets- och potentialprofilerna runt Cassini numeriskt med particle-in-cellsimuleringar för parametrar som modellerar hur rymdsonden rör sig relativt plasmat vid månen Enceladus bana.

 

Publisher
xi, 34 p.
Series
Trita-EE, ISSN 1653-5146
Identifiers
urn:nbn:se:kth:diva-12941 (URN)978-91-7415-673-7 (ISBN)
Presentation
2010-06-04, KTH, Stockholm, 10:00 (English)
Opponent
Supervisors
Note
QC 20100519Available from: 2010-05-19 Created: 2010-05-19 Last updated: 2012-03-21Bibliographically approved
2. Plasma and dust interaction in the magnetosphere of Saturn
Open this publication in new window or tab >>Plasma and dust interaction in the magnetosphere of Saturn
2012 (English)Doctoral thesis, comprehensive summary (Other academic)
Abstract [en]

The Cassini spacecraft orbits Saturn since 2004, carrying a multitude of instruments for studies of the plasma environment around the planet as well as the constituents of the ring system. Of particular interest to the present thesis is the large E ring, which consists mainly of water ice grains, smaller than a few micrometres, referred to as dust. The first part of the work presented here is concerned with the interaction between, on the one hand, the plasma and, on the other hand, the dust, the spacecraft and the Langmuir probe carried by the spacecraft. In Paper I, dust densities along the trajectory of Cassini, as it passes through the ring, are inferred from measured electron and ion densities. In Paper II, the situation where a Langmuir probe is located in the potential well of a spacecraft is considered. The importance of knowing the potential structure around the spacecraft and probe is emphasised and its effect on the probe's current-voltage characteristic is illustrated with a simple analytical model. In Paper III, particle-in-cell simulations are employed to study the potential and density profiles around the Cassini as it travels through the plasma at the orbit of the moon Enceladus. The latter part of the work concerns large-scale currents and convection patterns. In Paper IV, the effects of charged E-ring dust moving across the magnetic field is studied, for example in terms of what field-aligned currents it sets up, which compared to corresponding plasma currents. In Paper V, a model for the convection of the magnetospheric plasma is proposed that recreates the co-rotating density asymmetry of the plasma.

Place, publisher, year, edition, pages
Stockholm: KTH Royal Institute of Technology, 2012. xiii, 40 p.
Series
Trita-EE, ISSN 1653-5146 ; 2012:018
Keyword
saturn, dusty plasma
National Category
Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:kth:diva-93983 (URN)978-91-7501-343-5 (ISBN)
Public defence
2012-05-28, F3, Lindstedtsvägen 26, Stockholm, 10:00 (English)
Opponent
Supervisors
Note
QC 20120507Available from: 2012-05-07 Created: 2012-05-03 Last updated: 2012-05-07Bibliographically approved

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