Dissertations / Theses on the topic 'Ionospheric physics'
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Dorfman, Seth E. "Intense spreading of radar echoes from ionospheric plasmas." Thesis, Massachusetts Institute of Technology, 2005. http://hdl.handle.net/1721.1/32897.
Full textIncludes bibliographical references (leaf 41).
On December 25, 2004, a large-scale ionospheric plasma bubble was observed over Arecibo Observatory in Puerto Rico, inducing significant range spreading on ionograms. This phenomena may be explained by means of the E x B instability and gravitational Rayleigh-Taylor instability. A derivation of the dispersion relations for X and O mode waves transmitted from an ionosonde and an analysis of the collisional Rayleigh-Taylor instability leading to an expression for the growth rate are presented as background information. Ray tracing code developed by Nathan Dalrymple, a previous graduate student of Professor Min-Chang Lee, is extended, first to draw refractive index surfaces to illustrate a key principle in ray tracing and later to simulate range spreading due to depleted ionospheric ducts [1]. Data from Arecibo incoherent scatter radar and Arecibo's CADI digisonde is examined showing strong evidence for the development of a plasma bubble following a rise in the plasma layer and the appearance of a horizontal density gradient. In one portion of the ionosphere, this gradient is found to be at an angle of approximately 70 degrees to the Earth's magnetic field, a favorable condition for the excitation of the Rayleigh-Taylor instability over Arecibo.
by Seth E. Dorfman.
S.B.
Chapagain, Narayan P. "Dynamics of Equatorial Spread F Using Ground-Based Optical and Radar Measurements." DigitalCommons@USU, 2011. https://digitalcommons.usu.edu/etd/897.
Full textJensen, Joseph B. "The Effect of Ionospheric Conductivity on Magnetospheric Dynamics." Thesis, University of New Hampshire, 2018. http://pqdtopen.proquest.com/#viewpdf?dispub=10839528.
Full textThe connection between ionospheric conductivity and the dynamics of the magnetosphere was investigated, using several methods to change the ionospheric conductivity and then study the resultant changes to the magnetosphere. Computer simulations of the Earth's geospace environment were utilized using OpenGGCM coupled with an ionosphere model CTIM and a ring current model RCM.
Three methods were used to modify ionospheric conductivity. The incoming particle precipitation was modified by several orders of magnitude α = .01, .1, 1, 10, the ionospheric conductivity was increased or decreased by factors β = .25, .5, 1, 2, and 4, and for the last method differing values of F10.7, 70, 110, 150, 200, and 250 were used. Each of the methods is different because F10.7 mostly affects the dayside, while precipitation mostly affects the nightside, then using the β changes the conductivity over the whole ionosphere. This gives a good range for studying the effects of ionospheric conductivity on the magnetosphere.
The magnetospheric dynamics studied are: the dayside magnetopause location, the reconnection rate of the Earth's magnetosphere, X-line formation in the magnetotail, and substorm dynamics, both the frequency and magnitude of substorm occurrence.
To understand the effect of particle precipitation on conductivity two events were simulated, a calm period on 4 May 2005 and a strong storm period on 17 March 2013. Scaling the precipitation energy flux by several orders of magnitude, conductivities in the auroral oval were influenced which, in turn, influence the cross polar cap potentials. With the change in conductance, magnetospheric convection is enhanced or reduced, and the location of the subsolar distance of the magnetopause can change by up to one R E. The investigation of the reconnection rate for the varying precipitation simulations using the Hesse-Forbes-Bern method shows that particle precipitation affects the magnetic reconnection rate in these two events. The most notable differences, up to 40\%, occur on short time scales, that is, hours. A relation for longer time scales (tens of hours) between precipitation and reconnection for these two events is more difficult to ascertain. Differences in cross polar cap potential (CPCP) and reconnection rate (R) can be explained by viscous interactions and polar cap saturation. When precipitation was decreased, polar conductance was decreased, viscous interactions are stronger, and CPCP is higher than R. For high precipitation, high conductance cases the polar cap is in the saturation regime and CPCP is lower than R. Hemispheric asymmetries were found in the cross polar cap potential and in the calculated reconnection rate derived from the Northern and Southern Hemispheres. The majority of this research has already been published in the Journal of Geophysical Research: Space physics, "Particle Precipitation Effects on Convection and the Magnetic Reconnection Rate in Earth's Magnetosphere" https://doi.org/10.1002/2017JA024030.
For the whole ionospheric conductivity study, different values of β = .25, .5, 1, 2, 4 were used to modify the ionospheric conductivity after it had been calculated by the ionosphere model. A moderate storm period, 16 May 2011 was simulated. Many of the same conclusions found in the precipitation study were found in this study as well, such as, CPCP decreasing as conductivity increases, the point at which the polar cap saturates decreases with increasing conductivity, and reconnection rates change on short time scales, but the overall average rate remains very similar. The incoming precipitation was used to identify auroral brightening that is linked with substorms. The criteria for auroral brightenings used in this study is where the maximum precipitation increased by at least 1 mW/m2 within 20 minutes. The criteria for substorms is that the maximum precipitation increases by 80\% within 20 minutes. Identifying all the auroral brightenings and substorms showed that as conductivity increased the maximum amount of precipitation decreased, and also the number and frequency of both the substorms and auroral brightenings decreased. The occurrence of extended X-lines in the magnetotail was analyzed, where if an earthward flow of greater than 50 km/s extended for greater than 10 Re in YGSE was classified as an extended X-line. This is not to be confused with a bursty bulk flow or dipolarization front, which happen from reconnection but usually do not have a large extent in YGSE. Identifying extended X-lines in this manner showed a similar trend that as conductivity increased the number of extended X-lines decreased, and while there was not much of an indication if the size or location is affected much, the amount of time the simulation had extended X-lines present decreased.
For the F10.7 study, using values of 70, 110, 150, 200, and 250, the ionospheric conductivity was influenced mostly on the dayside. (Abstract shortened by ProQuest.)
Scherliess, Ludger. "Empirical Studies of Ionospheric Electric Fields." DigitalCommons@USU, 1997. https://digitalcommons.usu.edu/etd/6823.
Full textDe, Larquier Sebastien. "The mid-latitude ionosphere under quiet geomagnetic conditions: propagation analysis of SuperDARN radar observations from large ionospheric perturbations." Diss., Virginia Tech, 2013. http://hdl.handle.net/10919/24770.
Full textPh. D.
Pradipta, Rezy. "Incoherent scatter radar detection of enhanced plasma line in ionospheric E-region over Arecibo." Thesis, Massachusetts Institute of Technology, 2006. http://hdl.handle.net/1721.1/36122.
Full textIncludes bibliographical references (p. 45).
A series of incoherent scatter radar (ISR) observation were conducted at the Arecibo Observatory from December 27, 2005 until January 3, 2006. From plasma line measurements that were taken during this radar campaign, we found that plasma line enhancement was quite frequently seen in the ionospheric E-region. We hypothesized that the E-region plasma line enhancement over Arecibo was caused by precipitated electrons from the radiation belts. The precipitated electrons will enhance the population of suprathermal electrons in the E-region. Subsequently, suprathermal electrons will cause excitation of Langmuir waves that could be detected by incoherent scatter radar as plasma lines. In this thesis, we are going to examine and discuss the observed features of E-region plasma line enhancement over Arecibo to test this hypothesis. In addition, a theoretical discussion on Langmuir waves is also presented in a chapter of this thesis. Finally, we also introduce the Spread F Index (SFI) as a convenient bookkeeping method to summarize spread F condition over a certain period of time.
by Rezy Pradipta.
S.B.
Kane, Mark Vinton. "Transient subsurface features in Mars Express radar data: an explanation based on ionospheric holes." Thesis, University of Iowa, 2012. https://ir.uiowa.edu/etd/3477.
Full textNichols, James Warren. "The design of a new far ultraviolet interferometer for ionospheric spectroscopy." Thesis, Monterey, California : Naval Postgraduate School, 1990. http://handle.dtic.mil/100.2/ADA241767.
Full textThesis Advisor(s): Cleary, David D. ; Davis, D. Scott. "December 1990." Description based on title screen as viewed on April 2, 2010. DTIC Identifier(s): Ionosphere, Ultraviolet Spectroscopy, Interferometer. Author(s) subject terms: Ionosphere, Ultraviolet Spectroscopy, Interferometer. Includes bibliographical references (p. 64-67). Also available in print.
Subramanium, Mahesh. "A Study of the Gradient Drift Instability in the High-Latitude Ionosphere Using the Utah State University Time Dependent Ionospheric Model." DigitalCommons@USU, 1996. https://digitalcommons.usu.edu/etd/4869.
Full textLöfås, Henrik. "Ionospheric modification by powerful HF-waves : Underdense F-region heating by X-Mode." Thesis, Uppsala universitet, Institutionen för fysik och astronomi, 2008. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-121898.
Full textPraveen, Vikram. "Event Driven GPS Data Collection System for Studying Ionospheric Scintillation." Miami University / OhioLINK, 2011. http://rave.ohiolink.edu/etdc/view?acc_num=miami1323894410.
Full textRathod, Chirag. "Examining Plasma Instabilities as Ionospheric Turbulence Generation Mechanisms Using Pseudo-Spectral Methods." Diss., Virginia Tech, 2021. http://hdl.handle.net/10919/102892.
Full textDoctor of Philosophy
In the modern day, all wireless communication signals use electromagnetic waves that propagate through the atmosphere. In the upper atmosphere, there exists a region called the ionosphere, which consists of plasma (a mixture of ions, electrons, and neutral particles). Because ions and electrons are charged particles, they interact with the electromagnetic communication signals. A better understanding of ionospheric turbulence will allow for aid in forecasting space weather as well as improve future communication equipment. Communication signals become distorted as they pass through turbulent regions of the ionosphere, which negatively affects the signal quality at the receiving end. For a tangible example, when Global Positioning System (GPS) signals pass through turbulent regions of the ionosphere, the resulting position estimate becomes worse. This work looks at two specific causes of ionospheric turbulence: the gradient drift instability (GDI) and the Kelvin-Helmholtz instability (KHI). Under the correct background conditions, these instabilities have the ability to generate ionospheric turbulence. To learn more about the GDI and the KHI, a novel simulation model is developed. The model uses a method of splitting the equations such that the focus is on just the development of the turbulence while considering spatially constant realistic background conditions. The model is shown to accurately represent results from previously studied problems in the ionosphere. This model is applied to an ionospheric phenomenon known as subauroral polarization streams (SAPS) to study the development of the GDI and the KHI. SAPS are regions of the ionosphere with large westward velocity that changes with latitude. The shape of the latitudinal velocity profile depends on many other factors in the ionosphere such as the geomagnetic conditions. It is found that for certain profiles, the GDI will form in SAPS with some of these examples matching observational data. At higher altitudes, the model predicts that the KHI will form instead. While the model is applied to just the development of the GDI and the KHI in this work, it is written in a general manner such that other causes of ionospheric turbulence can be easily studied in the future.
Jenniges, Janelle V. "A Study of the Dayside High-Lattitude Ionospheric Electrodynamics During Extended Solar Minimum." DigitalCommons@USU, 2015. https://digitalcommons.usu.edu/etd/4481.
Full textLomidze, Levan. "The Role of Thermospheric Neutral Winds in the Mid-latitude Ionospheric Evening Anomalies." DigitalCommons@USU, 2015. https://digitalcommons.usu.edu/etd/4238.
Full textSantana, Julio III. "Investigating Ionospheric Parameters Using the Plasma Line Measurements From Incoherent Scatter Radar." Miami University / OhioLINK, 2012. http://rave.ohiolink.edu/etdc/view?acc_num=miami1344024880.
Full textNegale, Michael. "Investigating the Climatology of Mesospheric and Thermospheric Gravity Waves at High Northern Latitudes." DigitalCommons@USU, 2018. https://digitalcommons.usu.edu/etd/6937.
Full textTshisaphungo, Mpho. "Validation of high frequency propagation prediction models over Africa." Thesis, Rhodes University, 2010. http://hdl.handle.net/10962/d1015239.
Full textShim, JA Soon. "Analysis of Total Electron Content (TEC) Variations in the Low- and Middle-Latitude Ionosphere." DigitalCommons@USU, 2009. https://digitalcommons.usu.edu/etd/403.
Full textNorin, Lars. "Secondary Electromagnetic Radiation Generated by HF Pumping of the Ionosphere." Doctoral thesis, Uppsala universitet, Astronomi och rymdfysik, 2008. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-9393.
Full textTracy, Brian David. "Lunar Tidal Effects in the Electrodynamics of the Low-Latitude Ionosphere." DigitalCommons@USU, 2013. https://digitalcommons.usu.edu/etd/1968.
Full textFu, Haiyang. "Modeling of Plasma Irregularities Associated with Artificially Created Dusty Plasmas in the Near-Earth Space Environment." Diss., Virginia Tech, 2013. http://hdl.handle.net/10919/19248.
Full textPh. D.
Barabash, Victoria. "Investigation of Polar Mesosphere Summer Echoes in Northern Scandinavia." Doctoral thesis, Umeå University, Physics, 2003. http://urn.kb.se/resolve?urn=urn:nbn:se:umu:diva-176.
Full textThis PhD thesis deals with phenomena which are closely related to the unique thermal structure of the polar summer mesosphere, namely Polar Mesosphere Summer Echoes (PMSE). PMSE are strong radar echoes commonly observed by VHF MST radars from thin layers in the 80-90 km altitude interval at high latitudes during summer. They follow a seasonal pattern of abrupt appearance in late May and a gradual disappearance in mid-August. This period corresponds roughly to the time between the completion of the summer time cooling of the polar mesopause to the time of reversal of the mesospheric circulation to autumn condition. In this connection, PMSE are associated with the extremely low temperatures, i.e. below 140 K, which are unique to the polar summer mesopause. Traditional theories of radar (partial) reflection and scattering have been unable to explain the PMSE and the exact mechanism for their occurrence remains unclear despite the steadily increasing interest in them over the past 20 years. Currently accepted theories regarding the mechanism giving rise to PMSE agree that one of the conditions needed for enhanced radar echoes is the presence of low-mobility charge carries such as large cluster ions and ice aerosols which capture the ambient electrons. It has been established that the PMSE are in some way associated with noctilucent clouds (NLC), layers of ice crystals, which constitute the highest observed clouds in the earth’s atmosphere. PMSE occurrence and dynamics are also found to be closely connected with the planetary and gravity waves.
Observations of PMSE presented in this thesis have been carried out by the Esrange MST radar (ESRAD) located at Esrange (67°56’N, 21°04’E) just outside Kiruna in northernmost Sweden. The radar operates at 52 MHz with 72 kW peak power and a maximum duty cycle of 5%. The antenna consists of 12x12 array of 5-element Yagis with a 0.7l spacing. During the PMSE measurements the radar used a 16-bit complementary code having a baud length of 1mS. This corresponds to height resolution of 150 m. The sampling frequency was set at 1450 Hz. The covered height range was 80-90 km. The presence of PMSE was determined on the basis of the radar SNR (signal-to-noise ratio). The PMSE measurements have been made during May-August each year since 1997.
PMSE seasonal and diurnal occurrence rates as well as dynamics have been studied in connection with tidal winds, planetary waves, temperature and water vapor content in the mesosphere (Papers I, IV and VI). Simultaneous and common-volume observations of PMSE and noctilucent clouds have been performed by radar, lidar and CCD camera (Paper V). Correlation between variations in PMSE and variations in extra ionization added by precipitating energetic electrons or high-energy particles from the Sun has been examined (Papers II and III). Possible influence of transport effects due to the electric field on PMSE appearance has been studied during a solar proton event (Paper III).
Habarulema, John Bosco. "A contribution to TEC modelling over Southern Africa using GPS data." Thesis, Rhodes University, 2010. http://hdl.handle.net/10962/d1005241.
Full textHall, Jan-Ove. "Interaction between Electromagnetic Waves and Localized Plasma Oscillations." Doctoral thesis, Uppsala : Acta Universitatis Upsaliensis : Univ.-bibl. [distributör], 2004. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-4282.
Full textJorba, Ferro Oriol. "Étude de l'influence de la propreté électrostatique du satellite sur les mesures du champ électrique basse fréquence de TARANIS." Thesis, Toulouse, ISAE, 2018. http://www.theses.fr/2018ESAE0042/document.
Full textEarth-orbiting satellites travel in ionospheric plasma, a mixture of charged particles, and possibly neutral particles. Electrons and ions from this plasma, as well as Ultra-Violet (UV) emissions from the sun, interact with the surfaces of the satellite and modify its electrostatic charge. This loading can itself induce electrostatic discharges to the consequences ranging from electromagnetic disturbances (false commands for example) to the loss of the satellite. In low-Earth orbits (LEO), the kinetic and thermal energy of the plasma is generally low and therefore satellites rarely exhibit large discharges. Nevertheless, scientific missions that carry high-performance and accurate instruments can be affected by this satellite-plasma-UV-emissions interaction. This thesis is particularly interested in these phenomena of charge of the external structures of the satellite and the impact of this load on the scientific measurements carried out on board, i.e. measures of the electric field and the density of the thermal plasma
Liperovskaya, E. V., Claudia-Veronika Meister, M. Parrot, V. V. Bogdanov, and N. E. Vasil‘eva. "On Es-spread effects in the ionosphere connected to earthquakes." Universität Potsdam, 2006. http://opus.kobv.de/ubp/volltexte/2007/1500/.
Full textTalaee, Omid. "Distribution of Electron Temperatures in Titan's Lower Ionosphere." Thesis, Uppsala universitet, Institutionen för fysik och astronomi, 2013. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-194685.
Full textRosenqvist, Lisa. "Energy Transfer and Conversion in the Magnetosphere-Ionosphere System." Doctoral thesis, Uppsala University, Department of Astronomy and Space Physics, 2008. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-8716.
Full textMagnetized planets, such as Earth, are strongly influenced by the solar wind. The Sun is very dynamic, releasing varying amounts of energy, resulting in a fluctuating energy and momentum exchange between the solar wind and planetary magnetospheres. The efficiency of this coupling is thought to be controlled by magnetic reconnection occurring at the boundary between solar wind and planetary magnetic fields. One of the main tasks in space physics research is to increase the understanding of this coupling between the Sun and other solar system bodies. Perhaps the most important aspect regards the transfer of energy from the solar wind to the terrestrial magnetosphere as this is the main source for driving plasma processes in the magnetosphere-ionosphere system. This may also have a direct practical influence on our life here on Earth as it is responsible for Space Weather effects. In this thesis I investigate both the global scale of the varying solar-terrestrial coupling and local phenomena in more detail. I use mainly the European Space Agency Cluster mission which provide unprecedented three-dimensional observations via its formation of four identical spacecraft. The Cluster data are complimented with observations from a broad range of instruments both onboard spacecraft and from groundbased magnetometers and radars.
A period of very strong solar driving in late October 2003 is investigated. We show that some of the strongest substorms in the history of magnetic recordings were triggered by pressure pulses impacting a quasi-stable magnetosphere. We make for the first time direct estimates of the local energy flow into the magnetotail using Cluster measurements. Observational estimates suggest a good energy balance between the magnetosphere-ionosphere system while empirical proxies seem to suffer from over/under estimations during such extreme conditions.
Another period of extreme interplanetary conditions give rise to accelerated flows along the magnetopause which could account for an enhanced energy coupling between the solar wind and the magnetosphere. We discuss whether such conditions could explain the simultaneous observation of a large auroral spiral across the polar cap.
Contrary to extreme conditions the energy conversion across the dayside magnetopause has been estimated during an extended period of steady interplanetary conditions. A new method to determine the rate at which reconnection occurs is described that utilizes the magnitude of the local energy conversion from Cluster. The observations show a varying reconnection rate which support the previous interpretation that reconnection is continuous but its rate is modulated.
Finally, we compare local energy estimates from Cluster with a global magnetohydrodynamic simulation. The results show that the observations are reliably reproduced by the model and may be used to validate and scale global magnetohydrodynamic models.
Wilder, Frederick Durand. "Reverse Convection Potential Saturation in the Polar Ionosphere." Thesis, Virginia Tech, 2008. http://hdl.handle.net/10919/31847.
Full textMaster of Science
Liperovskaya, E. V., M. Parrot, V. V. Bogdanov, Claudia-Veronika Meister, M. V. Rodkin, and V. A. Liperovsky. "On long-term variations of foF2 in the mid-latitude ionosphere before strong earthquakes." Universität Potsdam, 2006. http://opus.kobv.de/ubp/volltexte/2007/1501/.
Full textHatch, Spencer Mark. "Stormtime and Interplanetary Magnetic Field Drivers of Wave and Particle Acceleration Processes in the Magnetosphere-Ionosphere Transition Region." Thesis, Dartmouth College, 2017. http://pqdtopen.proquest.com/#viewpdf?dispub=10603779.
Full textThe magnetosphere-ionosphere (M-I) transition region is the several thousand--kilometer stretch between the cold, dense and variably resistive region of ionized atmospheric gases beginning tens of kilometers above the terrestrial surface, and the hot, tenuous, and conductive plasmas that interface with the solar wind at higher altitudes. The M-I transition region is therefore the site through which magnetospheric conditions, which are strongly susceptible to solar wind dynamics, are communicated to ionospheric plasmas, and vice versa. We systematically study the influence of geomagnetic storms on energy input, electron precipitation, and ion outflow in the M-I transition region, emphasizing the role of inertial Alfven waves both as a preferred mechanism for dynamic (instead of static) energy transfer and particle acceleration, and as a low-altitude manifestation of high-altitude interaction between the solar wind and the magnetosphere, as observed by the FAST satellite. Via superposed epoch analysis and high-latitude distributions derived as a function of storm phase, we show that storm main and recovery phase correspond to strong modulations of measures of Alfvenic activity in the vicinity of the cusp as well as premidnight. We demonstrate that storm main and recovery phases occur during ~30% of the four-year period studied, but together account for more than 65% of global Alfvenic energy deposition and electron precipitation, and more than 70% of the coincident ion outflow. We compare observed interplanetary magnetic field (IMF) control of inertial Alfven wave activity with Lyon-Fedder-Mobarry global MHD simulations predicting that southward IMF conditions lead to generation of Alfvenic power in the magnetotail, and that duskward IMF conditions lead to enhanced prenoon Alfvenic power in the Northern Hemisphere. Observed and predicted prenoon Alfvenic power enhancements contrast with direct-entry precipitation, which is instead enhanced postnoon. This situation reverses under dawnward IMF. Despite clear observational and simulated signatures of dayside Alfvenic power, the generation mechanism remains unclear. Last, we present premidnight FAST observations of accelerated precipitation that is best described by a kappa distribution, signaling a nonthermal source population. We examine the implications for the commonly used Knight Relation.
Liperovsky, V. A., Claudia-Veronika Meister, L. N. Doda, E. V. Liperovskaya, V. F. Davidov, and V. V. Bogdanov. "On the possible influence of radon and aerosol injection on the atmosphere and ionosphere before earthquakes." Universität Potsdam, 2005. http://opus.kobv.de/ubp/volltexte/2007/1499/.
Full textKaeppler, Stephen Roland. "A rocket-borne investigation of auroral electrodynamics within the auroral-ionosphere." Diss., University of Iowa, 2013. https://ir.uiowa.edu/etd/2535.
Full textBorälv, Eva. "Substorm Features in the High-Latitude Ionosphere and Magnetosphere : Multi-Instrument Observations." Doctoral thesis, Uppsala universitet, Institutet för rymdfysik, Uppsalaavdelningen, 2003. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-3478.
Full textWohlwend, Christian Stephen. "Modeling the Electrodynamics of the Low-Latitude Ionosphere." DigitalCommons@USU, 2008. https://digitalcommons.usu.edu/etd/11.
Full textSazykin, Stanislav. "Theoretical Studies of Penetration of Magnetospheric Electric Fields to the Ionosphere." DigitalCommons@USU, 2000. https://digitalcommons.usu.edu/etd/7152.
Full textWilder, Frederick Durand. "The Non-Linear Electrodynamic Coupling Between the Solar Wind, Magnetosphere and Ionosphere." Diss., Virginia Tech, 2011. http://hdl.handle.net/10919/26586.
Full textPh. D.
Fathi, Pantea. "Ion-neutral reactions of C2H2N+ with hydrocarbons : relevant to Titan’s ionosphere." Licentiate thesis, Stockholms universitet, Fysikum, 2015. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-122952.
Full textHui, Debrup. "Altitudinal Variability of Quiet-time Plasma Drifts in the Equatorial Ionosphere." DigitalCommons@USU, 2015. https://digitalcommons.usu.edu/etd/4536.
Full textDavila, Ricardo Cruz. "A Study of Magnetic Activity Effects on the Thermospheric Winds in the Low Latitude Ionosphere." DigitalCommons@USU, 1994. https://digitalcommons.usu.edu/etd/6808.
Full textLannér, Viktor. "Incoherent Scattering of Twisted Radar Beams from the Ionosphere." Thesis, Uppsala universitet, Institutet för rymdfysik, Uppsalaavdelningen, 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-325768.
Full textMannix, Christopher Robert. "Measuring and modelling the impact of the ionosphere on space based synthetic aperture radars." Thesis, University of Birmingham, 2016. http://etheses.bham.ac.uk//id/eprint/6869/.
Full textMatalqah, Mohammed [Verfasser], Wolfgang [Gutachter] Stahl, and Erwin [Gutachter] Sedlmayr. "Development and experiments with the Ionospektroskop and a comparison with selected ionospheric parameters / Mohammed Matalqah ; Gutachter: Wolfgang Stahl, Erwin Sedlmayr." Berlin : Technische Universität Berlin, 2015. http://d-nb.info/1156274834/34.
Full textÅgren, Karin. "On the Formation and Structure of the Ionosphere of Titan." Doctoral thesis, Uppsala universitet, Institutionen för fysik och astronomi, 2012. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-172148.
Full textShebanits, Oleg. "Determination of Ion Number Density from Langmuir Probe Measurements in the Ionosphere of Titan." Thesis, Uppsala universitet, Institutionen för teknikvetenskaper, 2010. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-132567.
Full textSaturnus största måne Titan är ett väldigt intressant forskningsobjekt på grund av dess atmosfärs komplexa organiska kemi. Processer som pågår i Titans täta atmosfär kan hjälpa oss att förstå ursprunget till organiska föreningar på Jorden i dess unga ålder. Den internationella rymdsonden Cassini-Huygens blev uppskjuten mot Saturnus 1997, för att i detalj undersöka gasjätten och dess månar, speciellt Titan. Institutet för Rymdfysik (IRF) i Uppsala är ansvariga för operation och dataanalys av Langmuirsonden ombord Cassini som ligger i omloppsbanan kring Saturnus sedan 2004. Detta projekt omfattar analys av Langmuirsondens mätningar av Titans jonosfär från alla ”djupa” förbiflygningar av månen under perioden oktober 2004 – april 2010. Med hjälp av analysverktygen för Langmuirsonden, tas jonflödet fram efter kompensation för den atmosfäriska EUV extinktionen som ger upphov till fotoelektronströmmen från sonden. Fotoelektronströmmen som utsänds från proben ger en artefakt i data och måste (för detta projekt) korrigeras före analysen. Denna faktor är redan bestämd, men extinktionen av Titans atmosfär har endast korrigerats för i enstaka fall. Det korrigerade datat används för att få fram jondensiteten i Titans atmosfär genom att en genomsnittlig jonmass/höjd fördelning antas (jämförs med resultat från INMS-instrumentet) och kombineras med den beräknade hastighet som Cassini håller i banan genom jonosfären. Projektet utfördes vid Institutet för Rymdfysik, Uppsala.
Hammarsten, Michael. "A statistical study of incoherent scatter plasma line enhancements during the International Polar Year ’07-’08 in Svalbard." Thesis, Luleå tekniska universitet, Rymdteknik, 2016. http://urn.kb.se/resolve?urn=urn:nbn:se:ltu:diva-60158.
Full textSullivan, Joanna Mary. "Spectral studies of small-scale auroral structure and plasma instability in the high-latitude ionosphere." Thesis, University of Southampton, 2008. https://eprints.soton.ac.uk/65694/.
Full textKrämer, Eva. "Bow shock current closure to Earth's polar ionosphere - A statistical study using AMPERE and OMNI data." Thesis, Umeå universitet, Institutionen för fysik, 2021. http://urn.kb.se/resolve?urn=urn:nbn:se:umu:diva-184853.
Full textShebanits, Oleg. "Titan’s ionosphere and dust : – as seen by a space weather station." Doctoral thesis, Uppsala universitet, Institutet för rymdfysik, Uppsalaavdelningen, 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-329490.
Full textDe, Pascuale Sebastian. "The plasmasphere extension of Earth's atmosphere: a perspective from the Van Allen probes." Diss., University of Iowa, 2018. https://ir.uiowa.edu/etd/6405.
Full text