Готові списки джерел за темами / Planetary ions

Добірка наукової літератури з теми "Planetary ions"

Автор: Grafiati
Опубліковано: 23 вересня 2022
Оновлено: 28 січня 2023

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  1. Статті в журналах
  2. Дисертації
  3. Книги
  4. Частини книг
  5. Тези доповідей конференцій

Статті в журналах з теми "Planetary ions":

1

Dean Pesnell, W., and J. M. Grebowsky. "Meteoric ions in planetary ionospheres." Advances in Space Research 27, no. 11 (January 2001): 1807–14. http://dx.doi.org/10.1016/s0273-1177(01)00264-2.

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2

Kallio, Esa. "Escaping of planetary ions from Mars and Venus." Advances in Space Research 27, no. 11 (January 2001): 1815–24. http://dx.doi.org/10.1016/s0273-1177(01)00330-1.

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3

Strazzulla, G., J. R. Brucato, G. Cimino, G. Leto, and F. Spinella. "Interaction of solar wind ions with planetary surfaces." Advances in Space Research 15, no. 10 (January 1995): 13–17. http://dx.doi.org/10.1016/0273-1177(94)00145-q.

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4

Lilensten, J., C. Simon Wedlund, M. Barthélémy, R. Thissen, D. Ehrenreich, G. Gronoff, and O. Witasse. "Dications and thermal ions in planetary atmospheric escape." Icarus 222, no. 1 (January 2013): 169–87. http://dx.doi.org/10.1016/j.icarus.2012.09.034.

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5

Ibadov, Subhon. "On the production of multicharge ions in planetary nebulae." Proceedings of the International Astronomical Union 7, S283 (July 2011): 392–93. http://dx.doi.org/10.1017/s1743921312011581.

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AbstractProduction of multicharge ions due to generation of hot expanding plasma blobs, short-living “compound particles”, at high-velocity collisions between dust grains of a planetary nebula and dust particles of the interstellar medium is analytically considered. Dependence of the multiplicity of charge of produced ions on the relative velocity of colliding dust particles is determined.
6

Nahar, Sultana N. "Atomic Processes in Planetary Nebulae." Symposium - International Astronomical Union 209 (2003): 325–34. http://dx.doi.org/10.1017/s0074180900208942.

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A hot central star illuminating the surrounding ionized H II region usually produces very rich atomic spectra resulting from basic atomic processes: photoionization, electron-ion recombination, bound-bound radiative transitions, and collisional excitation of ions. Precise diagnostics of nebular spectra depend on accurate atomic parameters for these processes. Latest developments in theoretical computations are described, especially under two international collaborations known as the Opacity Project (OP) and the Iron Project (IP), that have yielded accurate and large-scale data for photoionization cross sections, transition probabilities, and collision strengths for electron impact excitation of most astrophysically abundant ions. As an extension of the two projects, a self-consistent and unified theoretical treatment of photoionization and electron-ion recombination has been developed where both the radiative and the dielectronic recombination processes are considered in an unified manner. Results from the Ohio State atomic-astrophysics group, and from the OP and IP collaborations, are presented. A description of the electronic web-interactive database, TIPTOPBASE, with the OP and the IP data, and a compilation of recommended data for effective collision strengths, is given.
7

Liu, Xiaowei. "Atomic processes in planetary nebulae." Proceedings of the International Astronomical Union 7, S283 (July 2011): 131–38. http://dx.doi.org/10.1017/s1743921312010836.

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AbstractProgress in the study of the atomic processes in planetary nebulae (PNe) is reviewed, focusing on the literature published since the last IAU symposium on PNe five years ago. High quality photoionization cross sections and recombination coefficients are now available for the first six ions of the trans-iron elements selenium and krypton, enabling robust modeling of their ionization structure and consequently converting the measured ionic abundances to elemental abundances. Major progress has been achieved in utilizing the recombination spectra of helium and heavy element ions to probe the nebular physical conditions. New ab initio, density-dependent effective recombination coefficients have been calculated for the recombination spectra of O ii and N ii, down to very low temperatures (~ 100–300 K). Plasma diagnostics based entirely on those heavy element recombination lines are developed and applied to the observations. It is shown that these heavy element recombination lines originate predominately from cold plasmas of temperatures ~ 1,000 K, in agreement with the predictions of the bi-abundance model that has been proposed to explain the dichotomy of nebular plasma diagnostics and abundance determinations using collisional excited lines (CELs) on the one hand and optical recombination lines (ORLs) on the other.
8

Delcourt, D. C. "On the supply of heavy planetary material to the magnetotail of Mercury." Annales Geophysicae 31, no. 10 (October 8, 2013): 1673–79. http://dx.doi.org/10.5194/angeo-31-1673-2013.

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Abstract. We examine the transport of low-energy heavy ions of planetary origin (O+, Na+, Ca+) in the magnetosphere of Mercury. We show that, in contrast to Earth, these ions are abruptly energized after ejection into the magnetosphere due to enhanced curvature-related parallel acceleration. Regardless of their mass-to-charge ratio, the parallel speed of these ions is rapidly raised up to ~ 2 VE × B (denoting by VE × B the magnitude of the local E × B drift speed), in a like manner to Fermi-type acceleration by a moving magnetic mirror. This parallel energization is such that ions with very low initial energies (a few tenths of eVs) can overcome gravity and, regardless of species or convection rate, are transported over comparable distances into the nightside magnetosphere. The region of space where these ions reach the magnetotail is found to extend over altitudes similar to those where enhanced densities are noticeable in the MESSENGER data, viz., from ~ 1000 km up to ~ 6000 km in the pre-midnight sector. The observed density enhancements may thus follow from E × B related focusing of planetary material of dayside origin into the magnetotail. Due to the planetary magnetic field offset, an asymmetry is found between drift paths anchored in the Northern and Southern hemispheres, which puts forward a predominant role of heavy material originating in the Northern Hemisphere in populating the innermost region of Mercury's magnetotail.
9

Thissen, Roland, Olivier Witasse, Odile Dutuit, Cyril Simon Wedlund, Guillaume Gronoff, and Jean Lilensten. "Doubly-charged ions in the planetary ionospheres: a review." Physical Chemistry Chemical Physics 13, no. 41 (2011): 18264. http://dx.doi.org/10.1039/c1cp21957j.

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10

Jarvinen, R., and E. Kallio. "Energization of planetary pickup ions in the solar system." Journal of Geophysical Research: Planets 119, no. 1 (January 2014): 219–36. http://dx.doi.org/10.1002/2013je004534.

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Статті в журналах

Дисертації з теми "Planetary ions":

1

Werner, Anita Linnéa Elisabeth. "Global and Time-dependent Modeling of Planetary Ions in Mercury's Magnetosphere." Thesis, Sorbonne université, 2021. http://www.theses.fr/2021SORUS527.

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L’environnement de Mercure est composé d’ions lourds originaires de l’atmosphère non-collisionnelle de Mercure (l’exosphère). La distribution spatiale des ions les plus abondants a été caractérisée par l’instrument « Fast Imaging Plasma Spectrometer (FIPS) » embarqué sur le satellite MESSENGER. Les modèles précédents de la distribution de la densité des ions planétaires dans la magnétosphère de Mercure ont prédits des densités pour les ions Na+ entre un à 3 ordres de grandeur différant de celles mesurées par FIPS. Cette thèse de doctorat décrit l’application d’un nouveau modèle numérique pour décrire les ions planétaires autour de Mercure, le Latmos IoniZed Exosphere Model (LIZE). LIZE est couplée à un modèle de l’exosphère (Exospheric Global Model; EGM) et un modèle magnétosphérique hybride (Latmos Hybrid Simulation; LatHyS). J’ai tout d’abord utilisé LIZE pour décrire la distribution des densités des ions Na+, O+ et He+ telle que mesurée par FIPS entre le 23 mars 2011 et le 30 avril 205. Nous avons pris en compte le champ de vue et la couverture en énergie de FIPS et avons simulé la fonction de distribution des vitesses. Ensuite, nous avons démontré que la réponse des espèces planétaires ioniques à un événement radiatif solaire intense était non-linéaire en fonction des espèces ioniques, de l’énergie, de la position dans la magnétosphère et de la position de la source de l’événement solaire à la surface du Soleil par rapport à Mercure. Le modèle LIZE permet une analyse originale des données FIPS et fournira des informations importantes sur le contexte des mesures qui vont être faites par la sonde BepiColombo
The Hermean environment contains heavy ions which have their origin in Mercury's collision-less atmosphere (exosphere). The spatial distribution of the most abundant ion species has been characterized by the Fast Imaging Plasma Spectrometer (FIPS) on the MESSENGER spacecraft. Previous models of the planetary ion density distribution in Mercury's magnetosphere produce Na+ densities which differ by 1-3 orders of magnitude from the FIPS observations. This thesis describes the application of a new ion density model, the Latmos IoniZed Exosphere model (LIZE). LIZE is coupled to a model of the exosphere (the Exospheric Global Model; EGM) and a hybrid magnetosphere model (Latmos Hybrid Simulation; LatHyS). I first use the LIZE model to reproduce the Na+-group, O+-group and He+ ion density distribution observed by FIPS between 23 March 2011 to 30 April 2015. We account for the FIPS field-of-view and energy range, and also simulate the 3-D ion phase space density distribution. I then use the time-dependent LIZE model to study the response of planetary ion species to a strong solar flare event. We demonstrate that the response of the planetary ion population in Mercury's magnetosphere to the flare is non-linear with respect to species, energy, location inside the magnetosphere and the location of the flare source region with respect to Mercury. The LIZE model offers a new capability for the analysis of FIPS data and will provide needed context to the ion measurements which will be made during the BepiColombo mission, which will be made from two different positions in space and by instruments with different spatial, temporal and energy coverage
2

Aizawa, Sae. "Transport and energization of planetary ions in the magnetospheric flanks of Mercury." Thesis, Sorbonne université, 2019. http://www.theses.fr/2019SORUS442.

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Dans cette thèse, par des méthodes numériques et l’analyse de données, le transport et l’accélération d’ions suite aux tourbillons KH qui peuvent se développer dans les flancs de la magnétosphère de Mercure sont examinés. Ici, l’échelle des variations du champ électrique peut être comparable à celle du mouvement de giration des ions lorsque les ions lourds d’origine planétaire (e.g., O^+, Na^+, ou K^+) se combinent à la complexité des champs électromagnétiques issus du développement des tourbillon KH. Les ions peuvent donc être accélérés de façon non-adiabatique lors de leur passage à travers la magnétopause de Mercure. Nous nous concentrons sur les effets des variations spatiale/temporelle du champ électrique le long du trajet ionique. Nos résultats montrent que l’intensification du champ, plutôt que le changement de son orientation, est responsable de l’accélération non-adiabatique à grande échelle des ions. Cette accélération se produit systématiquement pour les ions ayant des faibles énergies initiales dans la direction perpendiculaire au champ magnétique. Le gain énergétique étant du même ordre que l’énergie correspondant à la vitesse maximale de dérive ExB. Le transport des ions est aussi contrôlé par l’orientation du champ électrique de la magnetogaine. Comparant les données de MESSENGER, nous pouvons conclure que le nombre d’ion du groupe Na^+ détectés par FIPS augmente avec la présence d’ondes KH. Bien que nos résultats numériques supposent certaines différences dans la distribution énergétique des ions, nous n’avons pas trouvé de telles disparités. Pour mieux étudier ces conclusions, des études plus approfondies basées sur BepiColombo s’avèrent nécessaires
The transport and energization of planetary ions within Kelvin-Helmholtz (KH) vortices developing in the magnetospheric flanks of Mercury are investigated using both numerical methods and data analysis. Due to the presence of heavy ions of planetary origin (e.g., O^+, Na^+, and K^+) and the complicated field structure present during the KH vortex development, the scale of electric field variations can be comparable to that of the ion gyromotion. Therefore, ions may experience non-adiabatic energization as they drift across the magnetopause. In this study, we focus on the effects of the spatial/temporal variations of the electric field along the ion path. We show that the intensification, rather than the change in orientation, is responsible for large non-adiabatic energization of heavy ions of planetary origin. This energization systematically occurs for ions with low initial energies in the direction perpendicular to the magnetic field. The energy gain is of the order of the energy corresponding to the maximum ExB drift speed. It is also found that the ion transport across the magnetopause is controlled by the orientation of the magnetosheath electric field. Analyzing data from MESSENGER allow us to compare the observational facts with our numerical results. We find that the counts of Na^+-group detected by FIPS increase with the existence of KH waves, which is consistent with our numerical results. Although some differences in the energy distribution are expected in our numerical results, the data show no significant differences. This will be the subject of further studies using the newly developed BepiColombo instruments
3

Ricketts, Claire Louise. "The reactions of gas phase doubly-charged ions with neutral molecules of relevance to planetary ionospheres." Thesis, University of London, 2005. https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.497500.

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4

Cara, Antoine. "Développement d'un instrument compact pour la mesure des ions et électrons thermiques dans les environnements magnétosphériques." Thesis, Toulouse 3, 2018. http://www.theses.fr/2018TOU30046/document.

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L'instrument AMBRE 1 (Active Monitor Box of Electrostatic Risks) est un spectromètre de mesure du plasma (ions positifs et électrons) composé de deux têtes de mesure qui a été lancé à bord du satellite Jason 3 en Janvier 2016. A travers la mesure du plasma thermique (énergies comprises entre ~0 et 35 keV) cet instrument permet, d'une part, de déterminer la charge électrostatique des satellites et les populations en étant à l'origine pour répondre à des enjeux opérationnels, et d'autre part, de caractériser les environnements plasma magnétosphériques avec des enjeux scientifiques. La réduction des caractéristiques physiques (poids, consommation électrique et encombrement) des instruments AMBRE est un enjeu clé dans le but de rendre son embarquement systématique sur les plateformes satellites (scientifiques comme commerciales) et ainsi étendre le réseau de ce type de mesures dans l'environnement terrestre. L'objectif de cette thèse porte sur la conception, le développement et la réalisation d'un prototype d'instrument AMBRE 2 répondant à ces enjeux, tout en améliorant les performances scientifiques. Cette nouvelle génération d'instrument repose sur l'utilisation d'une seule tête qui mesure les deux types de population de manière alternée dans le temps. L'étude de chaque sous-système d'AMBRE 2 a permis de trouver les meilleurs compromis permettant de mesurer les deux types de population tout en minimisant les ressources allouées à l'instrument. Un prototype a été réalisé et testé sous vide avec un canon à ions et un canon à électron courant octobre 2017 afin de valider son principe de fonctionnement
The Active Monitor Box of Electrostatic Risks (AMBER) is a double-head thermal plasma (positive ions and electrons) electrostatic analyser that was launched onboard the Jason-3 spacecraft in January 2016. By measuring the thermal plasma (in the energy range ~0 - 45 keV) the instrument permits, on the one hand, to determine the spacecraft electrostatic charging and the populations at its origin with operational stakes, and, on the other hand, to characterize the magnetospheric plasma environments with scientific goals. Reducing the physical resources (weight, electric consumption, and volume) of the AMBRE line of instrument is key to a potential systematic embarkation onboard various platforms (scientific or commercial), thereby augmenting the constellation of such measurements in near-Earth space. The goal of the present thesis is to conceive, develop and build an AMBRE 2 instrument prototype that meets these goals while augmenting its scientific capabilities. This new generation of instrument relies on the use of a single head which alternatively measures ions and electrons. Each AMBRE 2 sub-system was studied and designed using the best trade-off solution between overall resources and capabilities. A prototype has been built and tested in a vacuum chamber with ion and electron beams in October 2017 in order to validate its functionality
5

Indrajith, Suvasthika. "Croissance moléculaire induite dans les agrégats d'hydrocarbures linéaires par la collision avec des ions et des électrons." Thesis, Normandie, 2021. http://www.theses.fr/2021NORMC201.

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Cette thèse est consacrée à l’étude expérimentale en phase gazeuse des collisions entre des particules ionisantes de faible énergie et des agrégats neutres d’hydrocarbures linéaires faiblement liés entre eux. Ces expériences ont eu comme objectif d’analyser les processus subséquents aux transferts d’énergie et de charge lors de la collision. Il s’agit de la fragmentation et de la croissance moléculaire via la mise en place de liaisons covalentes entre les molécules formant ces agrégats. Les travaux expérimentaux dans ce manuscrit ont permis d’éclairer les rôles respectifs de l’ionisation électronique et des pouvoirs d’arrêt nucléaire et électronique des projectiles sur la croissance au sein des agrégatsd’hydrocarbures linéaires. À cette fin, des études complémentaires ont été menées avec des faisceaux d’ions de basse énergies (keV) fournis par le GANIL (Caen), qui représente la majorité des résultats présentés, et des expériences utilisant des électrons ont aussi été réalisées à l’Institut de Chimie - Physique J.Heyrovsky (Prague, République Tchèque)
The work presented in this thesis concerns the experimental study in gas phase of the collisions between low energy ionizing particles and weakly bonded, neutral clusters of linear hydrocarbons. The purpose of these experiments was to analyze the processes subsequent to the energy and charge transfers during the collision, which are the fragmentation and molecular growth via the formation of covalently bonded molecules forming these clusters. The experimental work in this manuscript has shed light on the respective roles of electronic ionization and the nuclear and electronic stopping powers of projectiles on growth mecanisms within the clusters. To this end, the studies were carried out with low energy ion beams (keV) supplied by GANIL (Caen), which represents the majority of the results presented here, and experiments using electrons were also carried out at the J. Heyrovsky Institute of Chemistry - Physics (Prague, Czech Republic)
6

Wang, Zhiqiang. "Accélération Non Adiabatique des Ions causée par des Ondes électromagnétiques (Observations de Cluster et Double Star) et réponse du champ géomagnétique aux variations de la pression dynamique du vent solaire." Phd thesis, Université Paul Sabatier - Toulouse III, 2013. http://tel.archives-ouvertes.fr/tel-00843936.

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Cette thèse comporte deux thèmes principaux: l'un concerne l'accélération non adiabatique des ions dans la couche de plasma proche de la Terre, l'autre les pulsations géomagnétiques dues à la décroissance de la pression dynamique du vent solaire. L'accélération nonadiabatique des ions de la couche de plasma est importante pour comprendre la formation du courant annulaire et les injections énergétiques des sous-orages. Dans la première partie de cette thèse, nous présentons des études de cas d'accélération non adiabatique des ions de la couche de plasma observés par Cluster et TC-1 Double Star dans la queue magnétique proche de la Terre (par exemple à (X,Y, Z)=(-7.7, 4.6, 3.0) RT lors de l'évènement du 30 octobre 2006), beaucoup plus près de la Terre que ceux qui avaient été précédemment observés. Nous trouvons que les variations du flux d'énergie des ions, qui sont caractérisées par une décroissance entre 10 eV et 20 keV et une augmentation entre 28 keV et 70 keV, sont causées par l'accélération non adiabatique des ions associée étroitement avec les fortes fluctuations du champ électromagnétique autour de la gyrofréquence des ions H+. Nous trouvons aussi que les ions après l'accélération non adiabatique sont groupés en phase de gyration et c'est la première fois que ceci est trouvé dans la couche de plasma alors que cet effet a été observé dans le vent solaire dans les années 1980. Nous interprétons les variations de flux d'énergie des ions et les groupements en phase de gyration en utilisant un modèle non adiabatique. Les résultats analytiques et les spectres simulés sont en bon accord avec les observations. Cette analyse suggère que cette acceleration nonadiabatique associée aves les fluctuations du cham magnétique est un mécanisme efficace pour l'accélération des ions dans la couche de plasma proche de la Terre. Les structures de flux d'énergie présentées peuvent être uilisées comme un proxy pour identifier ce processus dynamique. Dans le deuxième thème, nous étudions la réponse du champ géomagnétique à une impulsion de la pression dynamique (Psw) du vent solaire qui a atteint la magnétosphère le 24 août 2005. En utilisant les données du champ géomagnétique à haute résolution fournies par 15 stations au sol et les données des satellites Geotail, TC-1 et TC-2, nous avons étudié les pulsations géomagnétiques aux latitudes aurorales dues à la décroissance brusque de Psw dans la limite arrière de l'impulsion. Les résultats montrent que la décroissance brutale de Psw peut exciter une pulsation globale dans la gamme de fréquence 4.3-11.6 mHz. L'inversion des polarisations entre deux stations des latitudes aurorales, la densité spectrale de puissance (PSD) plus grande près de la latitude de résonance et la fréquence augmentant avec la diminution de la latitude indiquent que les pulsations sont associées avec la résonance des lignes de champ (FLR). La fréquence résonante fondamentale (la fréquence du pic de PSD entre 4.3-5.8 mHz) dépend du temps magnétique local et est maximale autour du midi local magnétique. Cette caractéristique est due au fait que la dimension de la cavité magnétosphérique dépend du temps et est minimale à midi. Une onde harmonique est aussi observée à environ 10 mHz, qui est maximale dans le secteur jour, et est fortement atténuée lorsque on va vers le coté nuit. La comparaison entre les PSDs des pulsations provoquées pas l'augmentation brutale et la décroissance brutale de Psw montre que la fréquence des pulsations est inversement proportionnelle à la dimension de la magnétopause. Puisque la résonance des lignes de champ (FLR) est excitée par des ondes cavité compressée/guide d'onde, ces résultats indiquent que la fréquence de résonance dans la cavité magnétosphérique/guide d'onde est due non seulement aux paramètres du vent solaire mais est aussi influencée par le temps magnétique local du point d'observation.
7

Boldi, Robert A. (Robert Arthur). "A model of ion chemistry of electrified convection." Thesis, Massachusetts Institute of Technology, 1992. http://hdl.handle.net/1721.1/51502.

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Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Earth, Atmospheric, and Planetary Sciences, 1992.
Includes bibliographical references (leaves 175-182) and index.
by Robert A. Boldi.
Ph.D.
8

Jaïdane, Nejmeddine. "Etude du transfert de charge entre des atomes de soufre et des protons." Paris 7, 1987. http://www.theses.fr/1987PA077121.

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Calculs scf et ci des courbes de potentiel du systeme s+h**(+) dans les symetriplets pi et delta internenant dans la reaction, avec des orbitales moleculaires occupees representees par des orbitales atomiques polarisees et des orbitales moleculaires virtuelles donnees par la projection d'orbitales atomiques orthogonalement aux orbitales occupees. Traitement de la dynamique de l'echange de charge dans une representation diabatique ou les couplages radiaux sont nuls et l'echange de charge est induit par des couplages de type electronique. Construction d'une representation effective de dimension reduite au nombre des voies ouvertes; calcul des couplages radiaux. Resolution des equations de collision par un traitement quantique dans chaque symetrie; deduction de la constante de vitesse
9

Elder, Catherine Margaret. "The Effects of Melt on Impact Craters on Icy Satellites and on the Dynamics of Io's Interior." Diss., The University of Arizona, 2015. http://hdl.handle.net/10150/556825.

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Over the last fifty years, our knowledge of the Solar System has increased exponentially. Many planetary surfaces were seen for the first time through spacecraft observations. Yet the interiors of most planetary bodies remain poorly studied. This dissertation focuses on two main topics: the formation of central pit craters and what this reveals about the subsurface volatile content of the target material, and the mantle dynamics of Io and how they relate to the extensive volcanism on its surface. Central pit craters are seen on icy satellites, Mars, the Moon, and Mercury. They have terraced rims, flat floors, and a pit at or near their center. Several formation mechanisms have been suggested. This dissertation assesses the feasibility of central pit crater formation via drainage of impact melt through impact-generated fractures. For impacts on Ganymede, the expected volume of melt and volume of fracture space generated during the impact and the volume of melt able to drain before fractures freeze shut all exceed the observed central pit volumes on Ganymede. This suggests that drainage of impact melt could contribute to central pit crater formation on Ganymede. Molten rock draining through solid rock fractures will freeze shut more rapidly, so this work suggests that impact melt drainage is unlikely to be a significant factor in the formation of central pit craters on rocky bodies unless a significant amount of volatiles are present in the target. Io is the most volcanically active body in the Solar System. While volcanoes are most often associated with plate tectonics on Earth, Io shows no signs of plate tectonics. Previous work has suggested that Io could lose a significant fraction of its internal heat through volcanic eruptions. In this dissertation, I investigate the relationship between mantle convection and magma generation, migration by porous flow, and eruptions on Io. I couple convective scaling laws to a model solving the two-phase flow equations applied to a rising column of mantle. I show that Io has a partially molten upper mantle and loses the majority of its internal heat through volcanic eruption. Next, I present two-dimensional numerical simulations that self-consistently solve the two-phase flow equations including mantle convection and magma generation, migration by porous flow, and eruption. These simulations produce a high heat flux due to volcanic eruption, a thick lithosphere, a partially molten upper mantle, and a high eruption rate—all consistent with observations of Io. This model also reveals the eruption rate oscillates around the statistical steady state average eruption rate suggesting that the eruption rate and total heat flux measurements from the past 35 years may not be representative of Io's long term behavior.
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Ricketts, C. L. "The reactions of the molecular nitrogen doubly charged ion with neutral molecules of relevance to planetary ionospheres." Thesis, University College London (University of London), 2007. http://discovery.ucl.ac.uk/1445822/.

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Diatomic dications (e.g. C02+) have been known to exist for several decades and are believed to be important components of energised media. Molecular dications possess significant internal energy due to the Coulombic repulsion of their two positive charges, meaning that many possible reaction channels are available to dications in a collision with a neutral molecule. Modellers have recently predicted that N22+ is present in the ionosphere of Earth and Titan as well as the dications C > 22+ and 02+ in the ionosphere of Earth and CC > 22+ in the ionosphere of Mars. These recent predictions, of dications in planetary ionospheres, imply that dications, and processes involving dication-neutral collisions, may have more significance than previously thought in the upper atmospheres of planets. Therefore this thesis describes a study of the reactions between N2 dications and neutrals, potentially of relevance to the ionosphere of Earth and Titan. A position sensitive coincidence (PSCO) time-of flight (TOF) mass spectrometer is used to probe the reactivity, energetics and dynamics of the bimolecular reactions of N22 . Dication-neutrals reactions often result in a pair of singly charged ions. The PSCO experiment is used to collect these pairs of singly-charged ions in coincidence. From the position-sensitive data we extract the velocity vectors of the product ions, and if the reaction of interest involves the formation of a third, undetected, neutral species, its velocity can be determined via conservation of momentum. The electron transfer reactions between dications and neutrals have been well rationalized 2+ previously, so only the electron transfer reactions of N2 with Ne and NO are discussed in this thesis. This thesis concentrates on probing the less well rationalized, bond- forming reactions between dications and neutrals. The bond-forming reactions of N22+ with O2, CO2, H2O, C2H2, CH4, H2 and Ar have been investigated and discussed. Several new bond-forming reactions mechanisms are derived for example, the bond-forming reactions of N22+ with O2 proceed via a 'long' lived complex which dissociates via loss of a neutral and then charge separation, a mechanism which is also operating for one of the bond-forming reactions of N2 with CO2 and N2 with H2O. Additional bond-forming reactions are detected for N22+ with CO2 and H2O, which proceed via shorter lived collision complexes. The reactions of N22+ with C2H2, CH4, H2 and Ar all proceed via a variety of mechanisms involving short-lived collision complexes or H and electron stripping.

Книги з теми "Planetary ions":

1

Luhmann, Janet G. Assessment of ion scavenging processes at Venus and their evolutionary significance: Final technical report. [Washington, DC: National Aeronautics and Space Administration, 1996.

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2

Larson, Douglas J. Structure of the magnetotail current sheet. [Washington, DC: National Aeronautics and Space Administration, 1996.

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3

Smyth, William H. Studies for Io's extended atmosphere and neutral clouds and their impact on the local satellite atmosphere and on the planetary magnetosphere. [Washington, DC: National Aeronautics and Space Administration, 1993.

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4

United States. National Aeronautics and Space Administration., ed. Theoretical studies of interstellar processes: Final report, December 1, 1991-February 28, 1995. Lexington, MA: Institute for Scientific Research, 1995.

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5

Eland, John H. D., and Raimund Feifel. Molecules with four, five or seven atoms. Oxford University Press, 2018. http://dx.doi.org/10.1093/oso/9780198788980.003.0005.

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Double photoionisation spectra of NH3, C2H2, HCHO, C2N2, PCl3, CH4, the methyl halides CH3F, CH3Cl, CH3I, the methylene halides CH2Cl2, CH2Br2, CH2I2, the carbon tetrahalides CF4, CCl4, CBr4, germanium tetrahalides GeCl4, GeBr4, and SF6 are presented with analysis to identify the electronic states of the doubly charged ions. The effects of indirect double ionisation pathways are discussed. There are relatively few important molecules with just four atoms, but most of the ones included here are present and sometimes abundant in planetary and astrophysical environments. The range of five-atom molecules includes methane and all its simple derivatives. Where possible closely related molecules are grouped together in this chapter, as much of the discussion of their electronic structure is the same for all members of a group. This chapter also includes SF6 as a closely related molecule, even though its atom count goes beyond those of some molecules in later chapters.
6

Eland, John, and Raimund Feifel. Double Photoionisation Spectra of Molecules. Oxford University Press, 2018. http://dx.doi.org/10.1093/oso/9780198788980.001.0001.

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This book contains spectra of the doubly charged positive ions (dications) of some 75 molecules, including the major constituents of terrestrial and planetary atmospheres and prototypes of major chemical groups. It is intended to be a new resource for research in all areas of molecular spectroscopy involving high energy environments, both terrestrial and extra-terrestrial. All the spectra have been produced by photoionisation using laboratory lamps or synchrotron radiation and have been measured using the magnetic bottle time-of-flight technique by coincidence detection of correlated electron pairs. Full references to published work on the same species are given, though for several molecules these are the first published spectra. Double ionisation energies are listed and discussed in relation to the molecular electronic structure of the molecules. A full introduction to the field of molecular double ionisation is included and the mechanisms by which double photoionisation can occur are examined in detail. A preliminary chapter covers double photoionisation of an atom in order to explain the basic principles of the technique, then five chapters present spectra of molecules of increasing size. A seventh chapter on the new fields of core–core and core–valence double ionisations, with selected examples, completes the main body of the book. Appendices explain the detailed mechanisms of double photoionisation, the calibration of the electron spectrometers, and give a brief summary of the methods by which double ionisation energies are calculated theoretically.
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Rice University. Space Physics and Astronomy Dept. and United States. National Aeronautics and Space Administration., eds. Final report, entitled, Data reduction and analysis of Pioneer Venus Orbital Ion Mass Spectrometer: NASA grant NAG 2-566, covering the period October 1998 - March 1996. Houston, Tex: Space Physics and Astronomy Dept., Rice University, 1996.

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Частини книг з теми "Planetary ions":

1

Gaigalas, G., R. Kisielius, G. Merkelis, and M. Vilkas. "E2 and M1 Transition Probabilities in Ions of the Nitrogen Isoelectronic Sequence Calculated Using MBPT." In Planetary Nebulae, 95. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-2088-3_35.

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2

Ng, C. Y. "Absolute Total State-Selected Cross Sections for Ion-Molecule Reactions of Importance in Planetary Ionospheres." In Dissociative Recombination of Molecular Ions with Electrons, 401–14. Boston, MA: Springer US, 2003. http://dx.doi.org/10.1007/978-1-4615-0083-4_38.

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3

Avakyan, S. V., R. N. Il’in, V. M. Lavrov, and G. N. Ogurtsov. "Production of Electrons and Slow Ions by Electron Impact." In Collision Processes and Excitation of UV Emission from Planetary Atmospheric Gases, 37–89. London: Routledge, 2022. http://dx.doi.org/10.1201/9781315139685-2.

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4

Avakyan, S. V., R. N. Il’in, V. M. Lavrov, and G. N. Ogurtsov. "Production of Electrons and Slow Ions in Collisions of H+, H0 and He+ with Atmospheric Molecules and Atoms." In Collision Processes and Excitation of UV Emission from Planetary Atmospheric Gases, 91–142. London: Routledge, 2022. http://dx.doi.org/10.1201/9781315139685-3.

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5

Mihajlov, A. A., M. S. Dimitrijevic, and A. M. Ermolaev. "Radiation Charge Exchange and Radiation Ion-Atom Recombination as a Source of Continual E—M Radiation from Astrophysical Plasma." In Planetary Nebulae, 189. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-2088-3_61.

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6

Tripathi, S. N., M. Michael, and R. G. Harrison. "Profiles of Ion and Aerosol Interactions in Planetary Atmospheres." In Space Sciences Series of ISSI, 193–211. New York, NY: Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-87664-1_12.

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7

Gabrielse, Christine, Andrei Runov, Vassilis Angelopoulos, Emma Spanswick, and Drew L. Turner. "Premidnight Preponderance of Dispersionless Ion and Electron Injections." In Dawn-Dusk Asymmetries in Planetary Plasma Environments, 171–85. Hoboken, NJ, USA: John Wiley & Sons, Inc., 2017. http://dx.doi.org/10.1002/9781119216346.ch13.

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8

Berchem, Jean, Robert L. Richard, C. Philippe Escoubet, Simon Wing, and Frederic Pitout. "Large-Scale Simulations of Solar Wind Ion Entry and Dayside Precipitation." In Dawn-Dusk Asymmetries in Planetary Plasma Environments, 41–48. Hoboken, NJ, USA: John Wiley & Sons, Inc., 2017. http://dx.doi.org/10.1002/9781119216346.ch4.

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9

Fritz, Theodore A. "Ion Composition." In Physics of Solar Planetary Environments: Proceedings Of the International Symposium on Solar-Terrestrial Physics, June 7-18,1976 Boulder, Colorado Volume II, 716–29. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/sp008p0716.

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10

Kurosawa, Masanori, Hisayoshi Yurimoto, Kazuya Matsumoto, and Shigeho Sueno. "Hydrogen Analysis of Mantle Olivine by Secondary Ion Mass Spectrometry." In High-Pressure Research: Application to Earth and Planetary Sciences, 283–87. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm067p0283.

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Тези доповідей конференцій з теми "Planetary ions":

1

Shaposhnikov, V. E. "On the Origin of Io’s Ultraviolet Aurora." In Planetary Radio Emissions VII. Vienna: Austrian Academy of Sciences Press, 2011. http://dx.doi.org/10.1553/pre7s189.

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2

Nottoli, Emmanuelle, Philippe Bienvenu, Didier Bourlès, Alexandre Labet, Maurice Arnold, and Maité Bertaux. "Determination of Long-Lived Radionuclide (10Be, 41Ca, 129I) Concentrations in Nuclear Waste by Accelerator Mass Spectrometry." In ASME 2013 15th International Conference on Environmental Remediation and Radioactive Waste Management. American Society of Mechanical Engineers, 2013. http://dx.doi.org/10.1115/icem2013-96054.

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Radiological characterization of nuclear waste is essential for storage sites management. However, most of Long-Lived RadioNuclides (LLRN), important for long-term management, are difficult to measure since concentration levels are very low and waste matrices generally complex. In an industrial approach, LLRN concentrations are not directly measured in waste samples but assessed from scaling factors with respect to easily measured gamma emitters. Ideally, the key nuclide chosen (60Co, 137Cs) should be produced by a similar mechanism (fission or activation) as the LLRN of interest and should have similar physicochemical properties. However, the uncertainty on the scaling factors, determined from experimental and/or calculation data, can be quite important. Consequently, studies are performed to develop analytical procedures which would lead to determine precisely the concentration of LLRN in nuclear waste. In this context, the aim of this study was to determine the concentrations of three LLRN: 129I (T1/2 = 15.7×106 a), 41Ca (T1/2 = 9.94×104 a) and 10Be (T1/2 = 1.387×106 a) in spent resins used for primary fluid purification in Pressurized Water Reactors using Accelerator Mass Spectrometry (AMS) for measurement. The AMS technique combined mass spectrometry and nuclear physics to achieve highly efficient molecular and elemental isobars separation. Energies of several Million Electron-Volt transferred to the ions in the first accelerating part of specifically developed tandem accelerators lead to molecular isobars destruction through interaction with the argon gas used to strip the injected negative ions to positive ones. At the exit of the tandem accelerator, the energy acquired in both accelerating parts allows an elemental isobars separation based on their significantly different energy loss (dE) while passing through a thickness of matter dx that is proportional to their atomic number (Z) and inversely proportional to ions velocity (ν) according to the Bethe-Block law (1). (1)dEdx=k*Z2ν2 The use of a particle accelerator in conjunction with a selective ion source, mass and energy filters and a high-performance detector thus allow unambiguously identifying and measuring analyte concentration against much more abundant interfering isobars. The development of AMS and of related applications have recently been extensively reviewed [1–3]. Up to now, the potentialities of the accelerator mass spectrometry technique were explored for the measurement of cosmogenic radionuclides produced in the Earth’s environment either in the atmosphere or in the Earth’s crust (in situ-production). Many applications aiming to date and/or quantify Earth surface processes have been developed in the fields of geology, geomorphology and planetary sciences as well as archeology paleoanthropology and biomedicine. The present study extends the scope of AMS to nuclear industry. Because AMS facilities are not widely accessible and difficult to handle, LLRN concentrations in nuclear waste are usually determined using Inductively Coupled Plasma Mass Spectrometry (ICP-MS) and radiometric techniques. However for the measurement of very low LLRN concentrations, AMS becomes the most effective measurement method with detection limits of 105–106 atoms per sample. In this study, AMS measurements were performed using the French AMS national facility ASTER located at the Centre Européen de Recherche et d’Enseignement des Géosciences de l’Environnement (CEREGE). The challenge was to define a chemical treatment procedure allowing the measurement of the three nuclides, 10Be, 41Ca and 129I, by AMS. Each method selection was based on three main requirements: 1) a quantitative recovery in solution of Be, Ca, I and key radionuclides after resin mineralization, 2) a selective extraction from the sample matrix and the separation from β-γ emitters (3H, 14C, 55Fe, 59Ni, 60Co, 63Ni, 90Sr, 125Sb, 134Cs, 137Cs) and isobars, 3) the precipitation of each element under the best suited forms (i.e. AgI, CaF2, BeO) for AMS measurements. The chosen methods were optimized on synthetic solutions and finally applied for the determination of the three LLRN concentrations in spent resins from a 900 MWe Nuclear Power Reactor.
3

"Io's ultraviolet spot emission as a probe of the Jovian magnetic field model (abstract)." In Planetary Radio Emissions VIII. Vienna: Austrian Academy of Sciences Press, 2018. http://dx.doi.org/10.1553/pre8s169.

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4

Coates, Andrew J. "Ion pickup and acceleration: Measurements from planetary missions." In PHYSICS OF THE HELIOSPHERE: A 10 YEAR RETROSPECTIVE: Proceedings of the 10th Annual International Astrophysics Conference. AIP, 2012. http://dx.doi.org/10.1063/1.4723595.

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5

ASTON, G. "Ion propulsion technology requirements for planetary mission applications." In International Electric Propulsion Conference. Reston, Virigina: American Institute of Aeronautics and Astronautics, 1985. http://dx.doi.org/10.2514/6.1985-2000.

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6

Petrie, Simon, and Robert C. Dunbar. "Main Group Metal Ion Chemistry In Planetary Atmospheres." In ASTROCHEMISTRY: From Laboratory Studies to Astronomical Observations. AIP, 2006. http://dx.doi.org/10.1063/1.2359565.

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7

Mazelle, C. "Field-aligned and Gyrating Ion Beams in a Planetary Foreshock." In THE PHYSICS OF COLLISIONLESS SHOCKS: 4th Annual IGPP International Astrophysics Conference. AIP, 2005. http://dx.doi.org/10.1063/1.2032680.

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8

Choi, Michael K. "Using Paraffin PCM for Thermal Management of BOLAS Planetary CubeSats with Ion Thrusters." In AIAA Propulsion and Energy 2019 Forum. Reston, Virginia: American Institute of Aeronautics and Astronautics, 2019. http://dx.doi.org/10.2514/6.2019-4300.

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9

Das, Shounak, Cagri Kilic, Ryan Watson, and Jason Gross. "A Comparison of Robust Kalman Filters for Improving Wheel-Inertial Odometry in Planetary Rovers." In 34th International Technical Meeting of the Satellite Division of The Institute of Navigation (ION GNSS+ 2021). Institute of Navigation, 2021. http://dx.doi.org/10.33012/2021.17938.

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10

Choi, Michael K. "Correction: Using Paraffin PCM for Thermal Management of BOLAS Planetary CubeSats with Ion Thrusters." In AIAA Propulsion and Energy 2019 Forum. Reston, Virginia: American Institute of Aeronautics and Astronautics, 2019. http://dx.doi.org/10.2514/6.2019-4300.c1.

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