Thesis (M.S.)--University of wisconsin--Madison, 1982. / Typescript. eContent provider-neutral record in process. Description based on print version record. Includes bibliographical references.

Thesis (M.S.)--University of Wisconsin--Madison, 1984. / Typescript. eContent provider-neutral record in process. Description based on print version record. Includes bibliographical references (leaf 51).

At high winds, turbulence in the ocean surface mixed layer is dominated by organized coherent structures in the form of counterrotating helical vortices known as Langmuir cells. While the dynamics of the ocean surface layer has been studied rather extensively at lower wind speeds, the detailed physics at higher winds has remained largely inaccessible because of limited sea-going operations and difficulty conducting in situ measurements at high sea states. In the present thesis new measurement techniques, based on acoustical remote sensing, are described. A freely drifting imaging sonar was employed, which allowed us to follow time-evolving features for an extended period of time. This imaging sonar extends the acoustical approach beyond fixed orientation sonars and covers a full 360° circle on the surface. The full circle capability turns out to be a key addition to the measurements: it allowed quantitative evaluation of the directional properties of Langmuir circulation surface structure. These new methods allow us to sample near-surface circulation and bubble distributions even in extreme conditions, and contribute to our understanding of small scale dynamics in the wind driven surface layer. Using vertical velocity measurements in the convergent regions of Langmuir circulation and a model scaling, we infer the effective viscosity relevant to cell generation. Matching velocity- and temperature-inferred turbulent viscosities we estimate the depth scale over which the wind-wave forcing is of most importance. The velocity-inferred viscosity compares favorably with the mean model viscosity values evaluated at approximately two significant wave heights below the surface. Combining the effective viscosity calculated at different depths with the observed Stokes drift and friction velocity we estimate Langmuir numbers La between 0.015 and 0.1. We observe evolving cell patterns at larger La (between 0.02 and 0.05), which indicates that higher viscosity values than previously assumed in the models may be relevant for Langmuir circulation dynamics. Acoustical observations of the orientation of surface bubble clouds and the directional wave field during several deployments provided an opportunity for comparison of the directional properties of Langmuir circulation with a model that takes into account effects associated with misalignment of the Stokes drift and wind forcing. Model results imply that the growth rate is maximal overall when wind and waves are aligned. For a given angle between the Stokes drift and the wind (the misalignment angle) the direction of the cell axis for maximal growth lies between the Stokes drift and the wind and is mainly determined by (i) the misalignment angle and (ii) the ratio of the Stokes drift shear and mean Eulerian shear. Our ocean observations showed Langmuir cells responding to the changes in wind direction within 15 to 20 min. On two occasions, when the wind changed direction and waves lagged behind, the cells were observed to form in an intermediate direction (between wind and waves) consistent with model predictions. Observations of the near-surface circulation and thermal structure during a storm motivate analysis in terms of the Froude number derived from the measured vertical density gradient, the turbulent diffusivity which is inferred from the measured temperature distributions, and velocity and spatial structure of the circulation. The results demonstrate inhibition of Langmuir circulation by the presence of warm surface water at the beginning of a storm and provide a test of model description of the balance between wind-driven stirring and buoyant resistance. To better understand our measurements and the limitations of the approach, based on the acoustical backscatter, a technique for scatter location estimation is proposed. By comparing velocity magnitudes, independently measured with side-looking and upward-looking sonars, we estimate an effective scattering depth. These results show that the backscatter measured with side-looking sonars originates not right at the surface but at some depth below. / Graduate

The acceleration of electrons in a laser produced plasma wave was studied experimentally. A plasma with a modulated density was produced by illuminating a grating with a ruby laser at an intensity of 10¹⁰ W/cm². The plasma expanding above the surface of the grating was diagnosed using interferometry, shadowgraphy and Raman-Nath scattering. The plasma density was found to be modulated with an amplitude of [formula omitted]/n=8% for grating spacings ranging from 6 to 35 µm. A CO₂ laser of intensity 7xlO¹¹ W/cm2 then irradiated this modulated plasma and generated plasma waves. The phase speeds of the plasma waves are v[formula omitted] = ±[formula omitted]k[formula omitted], where k[formula omitted] is the wavenumber of the grating and [formula omitted] is the frequency of the CO₂ laser. Electrons were injected at an energy of 25 keV in one of the plasma waves. In order for the phase speed of the wave to synchronize with the accelerating electrons, a grating with constantly increasing line spacing was used. No conclusive evidence of electron acceleration was obtained, even after the injection energy was increased to 92 keV. This lack of evidence was the result of a large electric field perpendicular to the surface of the grating, which deflected the electrons onto the grating. This detrimental electric field is produced when fast electrons are emitted by the plasma and leave it positively charged. At the low laser intensity used in this experiment, the origin of these electrons could not be identified. Some techniques to remedy this difficulty are proposed. / Science, Faculty of / Physics and Astronomy, Department of / Graduate

The linearized Vlasov-Maxwell equations describing anisotropic plasma oscillations and waves are studied using an operator theoretic approach. The model considered is one dimensional so that after velocity averages perpendicular to this direction. have been taken, the equations can be naturally grouped into one set of equations for longitudinal modes and another set of equations for transverse modes. The problems of longitudinal and transverse plasma oscillations are studied by Fourier transforming the equations in the space variable and analyzing the resulting operator equations using the theory of semigroups. Existence and uniqueness theorems are proved, and solutions are constructed by the resolvent integration technique. The solutions are put into the form of a generalized eigenfunction expansion with eigenmodes corresponding to zeros of the appropriate plasma dispersion function. The expansion coefficients for eigenmodes corresponding to simple and second order real zeros of the plasma dispersion function are also presented, and constitute some of the new results obtained by our analysis. Existence and uniqueness of the solution to the longitudinal plasma wave boundary value problem is proved by writing the longitudinal equations in operator form and again using the theory of semigroups. The solution to the plasma wave boundary value problem is arrived at by a Fourier time transformation of the Vlasov equation coupled to Ampere's Law rather than Gauss‘ Law, and analyzing a scalar operator as opposed to the more complicated matrix operator that has previously been studied. Special care is used in constructing the half range transport operator whose resolution of the identity yields the solution in the form of a half range generalized eigenfunction expansion where again, new results are presented for the expansion coefficients for eigenfunctions corresponding to simple and second order real zeros of the fixed frequency longitudinal plasma dispersion function. Since this study is concerned with anisotropic plasmas, a non-even plasma equilibrium distribution function is assumed with the direct result that more stable and unstable plasma modes corresponding to real and complex zeros of the plasma dispersion function are possible that has previously been considered. Also, for the longitudinal plasma wave problem, the Wiener-Hopf factorization of the fixed frequency longitudinal plasma dispersion function is presented and the coupled nonlinear integral equations for the Wiener-Hopf factors are studied. These Wiener-Hopf factors are required in the construction of the half range transport operator. / Ph. D.

Thesis. 1978. Ph.D.--Massachusetts Institute of Technology. Dept. of Physics. / MICROFICHE COPY AVAILABLE IN ARCHIVES AND SCIENCE. / Bibliography: leaves 90-91. / Ph.D.

The Juno Waves instrument detected new broadband plasma wave emissions on the first three successful passes over the low altitude polar regions of Jupiter on Days 240 and 346 of 2016 and Day 033 of 2017. This study investigated the characteristics of these emissions and found similarities to whistler-mode auroral hiss observed at Earth, including the funnel-shaped frequency-time features. The electron cyclotron frequency was much higher than both the emission frequencies for all three days and the local plasma frequency, which was assumed to be 20 – 40 kHz. The electric to magnetic field (E/cB) ratio was around three near the start of each event and then decreased to one for the remaining duration of each pass. Spin modulation phase shifts were found on two of the three days (Day 240 and Day 033), indicating wave propagation up to the assumed plasma frequency. A correlation of the electric field spectral densities with the flux of up-going 20 to 800 keV electron beams on all three days were found, with correlation coefficients of 0.59, 0.72, and 0.34 for Day 240, Day 346, and Day 033 respectively. We conclude that the emissions are propagating in the whistler-mode and are driven by energetic up-going electron beams along the polar cap magnetic field lines.

Over the last fifty years, a multitude of spacecraft and rocket experiments have studied plasma wave emissions from Earth's auroral regions. One such emission is auroral hiss, a low-frequency whistler-mode wave that is produced in the auroral zone. Observations from Earth-orbiting spacecraft show that auroral hiss is generated by field-aligned electron beams, with the resulting plasma wave emission propagating along the resonance cone. This propagation results in auroral hiss appearing as a V-shaped funnel when observed on a frequency-time spectrogram. This thesis presents the first comprehensive study of auroral hiss at a planet other than Earth, using the Cassini spacecraft to study auroral hiss at Saturn. NASA's Cassini spacecraft, currently in orbit around Saturn, has allowed for the first opportunity to study this emission in detail at another planet. Since 2006, the Cassini spacecraft has twice been in a series of high inclination orbits, allowing investigation and measurements of Saturnian auroral phenomena. During this time, the Radio and Plasma Wave Science (RPWS) Investigation on Cassini detected low frequency whistler mode emissions propagating upward along the auroral field lines, much like terrestrial auroral hiss. Comparisons of RPWS data with observations from several other Cassini instruments, including the Dual-Technique Magnetometer (MAG), Magnetospheric Imaging Instrument (MIMI), and the Cassini Plasma Spectrometer (CAPS), have revealed a complete picture of this emission at Saturn. Observations from these instruments have been used to make a variety of determinations about auroral hiss at Saturn. RPWS has only observed this emission when Cassini was at high-latitudes, although these observations have shown no preference for local time. Tracking the times this emission has been observed revealed a clear periodicity in the emission. Further study later revealed not one but two rotational modulations, one in each hemisphere, rotating at rates of 813.9 and 800.7 degrees per day in the northern and southern hemispheres, respectively. These rates match with observations of the clock-like Saturn Kilometric Radiation. Study of the field-aligned current structures in the auroral regions revealed a strong upward-directed current in both hemispheres on the lower-latitude side of the auroral hiss emission. Along with correlating particle densities, these observations were used to infer the presence of a high-density plasmasphere at low latitudes, with the series of field-aligned current structures lining up with the outer boundary at L-shell values of around 12-15. Analysis of electron beams observed in conjunction with auroral hiss shows that these beams produce large growth rates for whistler-mode waves propagating along the resonance cone, similar to terrestrial auroral hiss. Analytical calculation of the normalized growth rates of ten electron beam events on Day 291, 2008, yielded a wide range of growth rates, from 0.004 to over 6.85 times the real frequency. The latter, a non-physical result, came from a violation of the weak growth approximation, suggesting there was so much growth that the analytical calculation was not valid in this instance. Numerical calculation using a plasma dispersion-solving code called WHAMP produced a growth rate of about 0.3, a still very large number, suggesting the detected beams may be the source of the observed auroral hiss plasma wave emission.

G. Bekefi, Sanborn C. Brown. / Reprinted from American journal of physics, v. 29, no. 7, 404-428, July, 1961. "February 14, 1961"--Cover. / Includes bibliographical references. / Army Signal Corps Contract DA36-039-sc-78108. Dept. of the Army Task 3-99-20-001 and Project 3-99-00-000.

The magnetosphere of pulsars is thought to consist of an electron-positron plasma rotating in the pulsar magnetic field (Beskin, Gurevich & Istomin 1983; Lominadze, Melikidze & Pataraya 1984; Gurevich & Istomin 1985). A finite, and indeed large, longitudinal electric field exists outside the star, and may accelerate particles, stripped from the surface, to high energies (Goldreich & Julian 1969; Beskin 1993). These particles may leave the magnetosphere via open magnetic field lines at the poles of the pulsar. This depletion of particles causes a vacuum gap to arise, a double layer of substantial potential difference. The primary particles, extracted from the star's surface, are accelerated in the double layer, along the pulsar magnetic field lines, and so produce curvature radiation. The curvature photons, having travelled the distance of the double layer may produce electron-positron pairs above the vacuum gap. These first-generation secondary particles, although no longer accelerating, may synchroradiate, generating photons which may then produce further electron-positron pairs. These synchrophoton produced pairs will be at energies lower than curvature photon produced pairs, since synchrophoton energies are approximately an order of magnitude less than that of the parent curvature photon. An attempt to model the electron-positron pulsar magnetosphere is made. A four component fluid electron-positron plasma is considered, consisting of a hot electron and positron species, at temperature Th , and a cool electron and positron species at temperature Tc . The hot components represent the parent first-generation curvature-born pairs, and the cooler components represent the second-generation pairs, born of synchrophotons. The hot components are assumed to be highly mobile, and are thus described by a Boltzmann density distribution. The cool components are more sluggish and are thus described as adiabatic fluids. The model is symmetric in accordance with pair production mechanisms, so that both species of hot(cool) electrons and positrons have the same temperature Th(Tc, and number density Nh(Nc ) . In the interests of completeness, linear electrostatic waves in five different types of electron-positron plasmas are considered. The dispersion relations for electrostatic waves arising in these unmagnetized plasmas are derived. Single species electron-positron plasmas are investigated, considering the constituents to be: both Boltzmann distributed; both adiabatic fluids; and finally, one species of each type. Linear electrostatic acoustic waves in multi-component electron-positron plasmas are then considered, under the four component model and a three component model (Srinivas, Popel & Shukla 1996). Small amplitude nonlinear electron-positron acoustic waves are investigated, under the four component electron-positron plasma model. Reductive perturbation techniques (Washimi & Taniuti 1966) and a derivation of the Korteweg-de Vries equation result in a zero nonlinear coefficient, and a purely dispersive governing wave equation. Higher order nonlinearity is included, leading to a modified Korteweg-de Vries equation (Watanabe 1984; Verheest 1988), which yields stationary soliton solutions with a sech dependence rather than the more familiar sech2. Arbitrary amplitude solitons are then considered via both numerical and analytical (Chatterjee & Roychoudhury 1995) analysis of the Sagdeev potential. The symmetric nature of the model leads to the existence of purely symmetrical compressive and rarefactive soliton solutions. Small and arbitrary amplitude soliton solutions are compared, and show good correlation. Under the assumption of Boltzmann distributed hot particles, severe restrictions are imposed on the existence domains of arbitrary amplitude soliton solutions. The Boltzmann assumption places a stringent upper limit on the cool species number density, in order for the solutions to be physical. An investigation is made of results obtained for an asymmetric electronpositron plasma (Pillay & Bharuthram 1992), consisting of cold electrons and positrons, and hot Boltzmann electrons and positrons at different temperatures Teh and Tph , and number density Neh and Nph . It is found that the assumption of Boltzmann particles again places restrictions on the acoustic soliton existence space, and that the results obtained may be physically invalid. Valid solutions are obtained numerically, within the boundaries of allowed cool species density values. / Thesis (M.Sc.)-University of Natal, Durban, 1998.