128 research outputs found
Multi‐instrument investigation of the location of Saturn's magnetotail x‐line
No full textReconnection is a fundamentally important process in planetary magnetospheres, with both local and global effects. At Saturn, observations of the magnetotail reconnection site (or x‐line) are rare, with only one in‐situ encounter reported to date. In this work, an extensive database of plasmoids and dipolarizations [Smith et al., 2016] was investigated from a multi instrument perspective in order to probe the location and variability of the magnetotail x‐line. Several clear intervals were identified in which the x‐line location could be indirectly inferred to move on relatively short timescales. Two case studies are presented, the first of which concerns short lived flows, suggesting the reconnection sites can be either short lived (∼10 minutes) or extremely azimuthally limited (∼3RS/0.4 hours of local time). The second interval concerns the tailward motion of the reconnection site (or sites), inferred from the increasing electron temperature (and diminishing electron density) associated with the flows. This tailward motion occurs over ∼2.5 hours (approximately a quarter of a planetary rotation). The composition of the suprathermal plasma suggests that this could be an example of the gradual depletion of mass loaded flux tubes (that must occur prior to lobe reconnection). These case studies are consistent with previous statistical work that suggested that the site of reconnection in the Kronian magnetotail can be highly dynamic
Dipolarization fronts with associated energized electrons in Saturn’s magnetotail
No full textWe present a statistical study of dipolarization fronts within Saturn’s magnetotail. Automated methods were used to identify 28 significant southward rotations of the field coupled with enhancements in the electron energy. The observed dipolarizations cover the majority of the magnetotail, though possess a strong dawn-dusk asymmetry (79% occur postmidnight). Almost half (43%) of dipolarizations occur within 3 hr of another event, though these chains are solely observed postmidnight. Most pitch angle distributions of the heated electron populations show increased relative fluxes parallel or perpendicular to the field, likely due to nonlocal heating effects. The electron temperature and density following the passage of a front are anticorrelated; the temperature increases are accompanied by a decrease in their density. The temperature increases by factors of 4–12, while the density drops by factors of 3–10. Premidnight events consistently show the smallest relative heating and density depletion, suggesting they are observed closer to their generation. In contrast, the location of the postmidnight x-line is inferred to be more variable, with a large variety of heating factors observed. Forty percent of the events show a strong reduction in water (W+) group fraction, likely related to either the preferential lossof equatorial heavy ions in departing plasmoids or the closure of open field. Two of these events show significant compositional changes suggesting the addition of plasma of external origin; we suggest that these events involved the closure of open field
Sources of local time asymmetries in magnetodiscs
No full textThe rapidly rotating magnetospheres at Jupiter and Saturn contain a near-equatorial thin current sheet over most local times known as the magnetodisc, resembling a wrapped-up magnetotail. The Pioneer, Voyager, Ulysses, Galileo, Cassini and New Horizons spacecraft at Jupiter and Saturn have provided extensive datasets from which to observationally identify local time asymmetries in these magnetodiscs. Imaging in the infrared and ultraviolet from ground- and space-based instruments have also revealed the presence of local time asymmetries in the aurora which therefore must map to local time asymmetries in the magnetosphere. Asymmetries are found in (i) the configuration of the magnetic field and magnetospheric currents, where a thicker disc is found in the noon and dusk sectors; (ii) plasma flows where the plasma flow has local time-dependent radial components; (iii) a thicker plasma sheet in the dusk sector. Many of these features are also reproduced in global MHD simulations. Several models have been developed to interpret these various observations and typically fall into two groups: ones which invoke coupling with the solar wind (via reconnection or viscous processes) and ones which invoke internal rotational processes operating inside an asymmetrical external boundary. In this paper we review these observational in situ findings, review the models which seek to explain them, and highlight open questions and directions for future work.</p
Survey of magnetosheath plasma properties at Saturn and inference of upstream flow conditions
No full textA new Cassini magnetosheath data set is introduced that is based on a comprehensive survey of intervals in which the observed magnetosheath flow was encompassed within the plasma analyzer field of view and for which the computed numerical moments are therefore expected to be accurate. The data extend from 2004 day 299 to 2012 day 151 and comprise 19,155 416 s measurements. In addition to the plasma ion moments (density, temperature, and flow velocity), merged values of the plasma electron density and temperature, the energetic particle pressure, and the magnetic field vector are included in the data set. Statistical properties of various magnetosheath parameters, including dependence on local time, are presented. The magnetosheath field and flow are found to be only weakly aligned, primarily because of a relatively large z component of the magnetic field, attributable to the field being pulled out of the equatorial orientation by flows at higher latitudes. A new procedure for using magnetosheath properties to estimate the upstream solar wind speed is proposed and used to determine that the amount of electron heating at Saturn's high Mach-number bow shock is ~4% of the dissipated flow energy. The data set is available as supporting information to this paper.</p
Dipolarization Fronts With Associated Energized Electrons in Saturn's Magnetotail
No full textWe present a statistical study of dipolarization fronts within Saturn's magnetotail. Automated methods were used to identify 28 significant southward rotations of the field coupled with enhancements in the electron energy. The observed dipolarizations cover the majority of the magnetotail, though possess a strong dawn‐dusk asymmetry (79% occur postmidnight). Almost half (43%) of dipolarizations occur within 3 hr of another event, though these chains are solely observed postmidnight. Most pitch angle distributions of the heated electron populations show increased relative fluxes parallel or perpendicular to the field, likely due to nonlocal heating effects. The electron temperature and density following the passage of a front are anticorrelated; the temperature increases are accompanied by a decrease in their density. The temperature increases by factors of 4–12, while the density drops by factors of 3–10. Premidnight events consistently show the smallest relative heating and density depletion, suggesting they are observed closer to their generation. In contrast, the location of the postmidnight x‐line is inferred to be more variable, with a large variety of heating factors observed. Forty percent of the events show a strong reduction in water (W+) group fraction, likely related to either the preferential loss of equatorial heavy ions in departing plasmoids or the closure of open field. Two of these events show significant compositional changes suggesting the addition of plasma of external origin; we suggest that these events involved the closure of open field
Spin-Echo aufgelöste Neutronenstreuung von selbstorganisierten Polymergrenzflächen
No full textThis thesis focused on two main objectives: First, the clarification of the prospects of the spin-echo resolved grazing incidence neutron scattering method (SERGIS) for the investigation of buried interfaces. And second, the investigation of the self-organisation (i.e. microphase separation and dewetting) of ultrathin poly(styrene-block-isoprene) diblock copolymer films on silicon substrates by means of SERGIS and complementary techniques.
SERGIS is a novel neutron scattering technique which was implemented and further developed at the new neutron / x-ray reflectometer N-REX+ at the FRM II (Garching, Germany). In contrast to conventional small-angle scattering methods, SERGIS characterises the lateral structure and morphology of interfaces and thin-film systems in real space. The technique uses a polarised primary beam, and the measured quantity is the integral polarisation of the scattered beam. By decoupling the measurement resolution and the beam divergence (in a first approximation), SERGIS aims at a good resolution and a good measurement statistics simultaneously.
As a first systematic application of SERGIS to a real physical problem, the dewetting and internal structure of ultrathin poly(styrene-block-isoprene) diblock copolymer films were studied by means of SERGIS and complementary surface sensitive techniques, namely neutron and x ray reflectivity and atomic force microscopy (AFM).Diese Dissertation widmet sich zwei Forschungsschwerpunkten: Erstens, den Möglichkeiten und Grenzen der Spin-Echo aufgelösten Neutronen Streuung (SERGIS) zur Untersuchung von verborgenen Grenzflächen. Und zweitens, der Untersuchung von Selbstorganisation (Mikrophasenseparation und Entnetzen) sehr dünner poly(styrol-block-isopren) Diblock Copolymer Filme auf Siliziumsubstrat mittels SERGIS und komplementärer Methoden.
SERGIS ist eine neue Neutronenstreumethode, die am neuen Neutronen- / Röntgen-Reflektometer N REX+ am FRM II (Garching, Deutschland) implementiert und weiterentwickelt wurde. Im Gegensatz zu konventionellen Neutronen Kleinwinkelstreumethoden, wird mittels SERGIS die laterale Struktur und Morphologie an Grenzflächen und Dünnfilmsystemen im Realraum charakterisiert. Die Messgröße ist die Depolarisierung eines zu Beginn vollständig polarisierten Neutronenstrahls. In dem die Auflösung und die Strahldivergenz in erster Ordnung entkoppelt sind, soll sowohl eine gute Auflösung als auch eine gute Statistik erreicht werden.
Als erste systematische Anwendung von SERGIS an einem physikalischen Problem wurde das Entnetzen und die interne Struktur von sehr dünnen Poly(Styrol-block-Isopren) Diblock Copolymer Filmen mittels SERGIS und komplementären oberflächensensitiven Methoden, wie Neutronen- und Röntgen-Reflektivität als auch Raster-Kraft-Mikroskopie (AFM) untersucht
A combined model of pressure variations in Titan's plasma environment
No full textIn order to analyze varying plasma conditions upstream of Titan, we have combined a physical model of Saturn?s plasma disk with a geometrical model of the oscillating current sheet. During modeled oscillation phases where Titan is farthest from the current sheet, the main sources of plasma pressure in the near-Titan space are the magnetic pressure and, for disturbed conditions, the hot plasma pressure. When Titan is at the center of the sheet, the main sources are the dynamic pressure associated with Saturn?s cold, subcorotating plasma and the hot plasma pressure under disturbed conditions. Total pressure at Titan (dynamic plus thermal plus magnetic) typically increases by a factor of up to about 3 as the current sheet center is approached. The predicted incident plasma flow direction deviates from the orbital plane of Titan by ≲ 10◦ . These results suggest a correlation between the location of magnetic pressure maxima and the oscillation phase of the plasma sheet. Our model may be used to predict near-Titan conditions from ?far-field? in situ measurements.Fil: Achilleos, N.. University College London; Reino UnidoFil: Arridge, C. S.. University College London; Reino UnidoFil: Bertucci, Cesar. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Guio, P.. University College London; Reino UnidoFil: Romanelli, Norberto Julio. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Sergis, N.. Academy Of Athens. Office for Space Research and Technology; Greci
Dynamical theory: Application to spin-echo resolved grazing incidence scattering from periodic structures
No full textNeutron spin-echo resolved grazing incidence scattering (SERGIS) measurements performed on a silicon diffraction grating with a rectangular profile were shown in our previous publications to be well explained by dynamical theory calculations. The theory is based on a Bloch wave expansion of the neutron wavefunction in the periodic layer of the grating, which includes all multiple scattering within that layer. Calculations show that the spin-echo polarization should be very sensitive to the scattering geometry (i.e., incident angle, sample alignment and beam divergence) and the sample specifications (i.e., grating period, groove depth). To test these predictions, SERGIS measurements have been performed on a set of gratings with different specifications in various scattering geometries. In all cases, simulations based on the dynamical theory, with all the parameters set to their known values, are in good agreement with the collected data.RRR/Radiation, Radionuclides and ReactorsApplied Science
Upstream of Saturn and Titan
No full textThe formation of Titan's induced magnetosphere is a unique and important example in the solar system of a plasma-moon interaction where the moon has a substantial atmosphere. The field and particle conditions upstream of Titan are important in controlling the interaction and also play a strong role in modulating the chemistry of the ionosphere. In this paper we review Titan's plasma interaction to identify important upstream parameters and review the physics of Saturn's magnetosphere near Titan's orbit to highlight how these upstream parameters may vary. We discuss the conditions upstream of Saturn in the solar wind and the conditions found in Saturn's magnetosheath. Statistical work on Titan's upstream magnetospheric fields and particles are discussed. Finally, various classification schemes are presented and combined into a single list of Cassini Titan encounter classes which is also used to highlight differences between these classification schemes.</p
Titan's interaction with the supersonic solar wind
No full textAfter 9 years in the Saturn system, the Cassini spacecraft finally observed Titan in the supersonic and super-Alfvénic solar wind. These unique observations reveal that Titan?s interaction with the solar wind is in many ways similar to unmagnetized planets Mars and Venus and active comets in spite of the differences in the properties of the solar plasma in the outer solar system. In particular, Cassini detected a collisionless, supercritical bow shock and a well-defined induced magnetosphere filled with mass-loaded interplanetary magnetic field lines, which drape around Titan?s ionosphere. Although the flyby altitude may not allow the detection of an ionopause, Cassini reports enhancements of plasma density compatible with plasma clouds or streamers in the flanks of its induced magnetosphere or due to an expansion of the induced magnetosphere. Because of the upstream conditions, these observations may be also relevant to other bodies in the outer solar system such as Pluto, where kinetic processes are expected to dominate.Fil: Bertucci, Cesar. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Hamilton, D. C.. University of Maryland; Estados UnidosFil: Kurth, W. S.. University of Iowa; Estados UnidosFil: Hospodarsky, G.. University of Iowa; Estados UnidosFil: Mitchell, D.. University Johns Hopkins; Estados UnidosFil: Sergis, N.. Academy of Athens; GreciaFil: Edberg, N. J. T.. Swedish Institute of Space Physics,; SueciaFil: Dougherty, M. K.. Imperial College London; Reino Unid
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