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La première partie de cette thèse présente une modélisation des émissions aurorales de Jupiter dans l'ultraviolet. Le but de ce travail est de quantifier comment ces émissions permettent de contraindre l'énergie des électrons qui précipitent dans la haute atmosphère polaire de la planète. Deux types d'émissions sont étudiés : celle de la raie Lyman alpha de l'hydrogène atomique ainsi que celles de H2. Les précipitations d'électrons aurorales sont modélisées à l'aide d'un code de transport cinétique. Le profil et l'intensité de la raie H Lyman alpha sont obtenus avec un code de transfert radiatif. Des spectres synthétiques des émissions de H2 sont calculés. En étudiant la variabilité des raies en fonction de l'énergie des électrons nous montrons que seules des observations à très haute résolution permettront de contraindre fortement les précipitations d'électrons. La deuxième partie de cette thèse présente la première modélisation de l'émission H Lyman alpha d'un Jupiter chaud jamais réalisée. Si elle était détectée, cette raie permettrait de caractériser l'environnement des planètes extrasolaires. L'émission de l'étoile est beaucoup plus intense que celle de la planète, ce qui rend la détection de la raie planétaire très difficile. Les seules estimations de contraste qui avaient été réalisées jusqu'à présent découlaient d'extrapolations basées sur l'émission de Jupiter. Nous introduisons ici des outils appropriés au calcul des émissions des Jupiter chauds, en tenant compte des spécificités de leur haute atmosphère, et notamment leur forte ionisation et leurs températures qui dépassent les 10 000 K. Nous évaluons l'émission Lyman alpha de deux Jupiter chauds, en tenant compte de plusieurs sources d'excitation des particules : les émissions aurorales et thermiques sont calculées, ainsi que l'émission excitée par le rayonnement de l'étoile. Nous montrons que, dans le cas du Jupiter chaud HD 209458b, la détection de l'émission planétaire n'est pas possible avec les instruments actuels. En revanche la raie Lyman alpha du Jupiter chaud HD 189733b semble pouvoir être détectée avec l'instrument STIS du télescope spatial Hubble. / The first part of this thesis describes a modeling of the auroral emission of Jupiter in the ultraviolet. The aim of this work is to quantify how these emissions allow to constrain the energy of the electrons that precipitate in the upper atmosphere of the planet at polar latitudes. Two kinds of emissions are studied : the one of the Lyman alpha line of atomic hydrogen and those of H2. The auroral electron precipitation is modeled with a kinetic transport code. The H Lyman alpha line profile and intensity are obtained with a radiative transfer code. Synthetic spectra of H2 emissions are calculated. By studying the variability of the lines as a function of the energy of the precipitating electrons, we show that only high resolution observations will allow to put strong constraints on the electron precipitation. The second part of this thesis presents the first calculation of the H Lyman alpha emission of a hot Jupiter ever realized. If it were detected, this line would allow to constrain the environment of the extrasolar planets. The stars' emission is much more intense than that of the planet, which transforms the detection of the planetary line in a very difficult challenge. Up to now, the only estimations of contrast that have been realized are based on extrapolations of Jupiter's emission. Here we present tools that are adequate to calculate the emission of hot Jupiters. They take into account the particularities of their atmosphere, like their high ionization degree and their temperatures that exceed 10,000 K. We calculate the Lyman alpha emission of two hot Jupiters, by taking into account the auroral, thermal and dayglow contributions. In the case of the hot Jupiter HD 209458b, we show that current facilities do not allow to detect the planetary emission. On the other hand, the detection of the Lyman alpha line of the planet HD 189733b seems to be within reach of the Hubble Space Telescope.

This thesis explores the eighteenth-century aesthetic of the sublime in application to Mozart’s Symphony No. 41 Jupiter, K. 551. Using Immanuel Kant’s definition of the mathematical sublime and Johan Georg Sulzer’s idea of the sublime, I argue that Mozart achieves this aesthetic through the synthesis of stylistic opposites: the learned and the galant. The culmination of such is best articulated in the fugue found in the Coda of the fourth movement. In this segment, Mozart combines five galant motives into a learned fugue; this intricate combination of stylistic opposites creates an elevated effect, one in keeping with eighteenth-century philosophies of the sublime. Drawing from my own experiences, I further argue for the subjectivity of the sublime and discuss its occurrence both in composition and as emotion.

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Pioneer 10 and 11 polarimetry maps of Jupiter, taken at a wide variety of phase angles, have been analyzed. Data were reduced in two colors for Jupiter's South Equatorial Belt (latitude -5 to -8 degrees) and scattering models were constructed. Variations in polarization from center to limb set constraints on the vertical structure of the atmosphere. The absolute polarization near the center of the disc constrained the single scattering polarization phase matrix of the scattering particles. After exploring several types of cloud models, it was found that a two cloud model with a haze in the upper atmosphere fits the data best. Several types of vertical structures were ruled out, including gas over a nonpolarizing Lambert surface, gas over a polarizing cloud deck, uniformly mixed gas with scattering particles (Reflecting Scattering Model), and models where the cloud tops diffusely mixed with gas as a function of altitude. Constraints have been set upon the polarimetric scattering properties of the haze and lower clouds. The haze particles are closely approximated by conservatively scattering spheres of index of refraction 1.5 and uniformly distributed sizes between 0.16 and 0.18 microns radius. A relationship exists between the required index of refraction for the haze particles and the mean size of the particles. It is possible that the particles are more broadly distributed in size, as this area was not extensively explored. The optical depth of the haze is between 0.125 and 0.250 at a wavelength of 0.44 microns, and lies near the 200 millibar pressure level. The upper cloud, which is thought to be made of ammonia crystals, must be at least optical depth 2, and could be semi-infinite. The polarization scattering properties of the clouds are distinctly different from the haze, indicating a compositional or size difference. The cloud particles have polarizing properties indicative of large (larger than 0.5 micron radius) particles. The upper cloud has been modelled to be near the 500 millibar level, but the pressure level for the best fitting model depends upon the chosen single scattering phase matrix. For more negatively polarizing cloud particles, the cloud would be located deeper in the atmosphere. The lowest cloud is more weakly constrained. Its scattering properties are set the same as the upper cloud, and it has been modelled as having semi-infinite optical depth. For the nominal scattering phase matrix, this cloud is located near the 2250 millibar pressure level. The constraints set on both the vertical structure and the particle scattering properties can be useful in the determination of Jupiter's solar flux deposition profile. Additionally, the location of the cloud and haze layers in Jupiter's atmosphere is important to the understanding of the heat balance of the planet, as well as to the understanding of the global dynamic of Jupiter's atmosphere.

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Jupiter, the largest planet in the solar system, is not only an emitter of thermal radiation like any other planet. Jupiter also emits relatively high-intensity non-thermal radiation in two bands, the decimetre wavelength range and the decametre wavelength range (5 MHz< f < 40 MHz). The decimetric radiation is believed to be due to synchrotron radiation of electrons trapped in a kind of Jovian "Van Allen belt". This thesis deals almost exclusively with the decametric radiation. Although the decametric radiation has been observed for 15 years since its discovery by Burke and Franklin in 1955, there is no generally accepted theoretical model of its generation to be found in the literature as yet. This is not surprising, as there are many complex and confusing aspects of the radiation. And since our knowledge of the Jovian ionosphere, magnetosphere and magnetic field is very limited indeed, every theoretical model must be based on some more or less well justified assumptions. It is, however, possible to draw some conclusions from the observed properties of the decimetric and decametric radiation. The radiation in both bands is polarized. It has been shown that at least part of the polarization is an intrinsic property of the radiation source at Jupiter, This indicates the existence of a Jovian magnetic field. The magnitude and shape of the magnetic field, however, is open to discussion, although a dipole field does seem to be a good approximation at least for large distances from Jupiter. Intro. p. 1-2.

The Juno spacecraft has measured Jupiter's low-order, even gravitational moments, J(2)-J(8), to an unprecedented precision, providing important constraints on the density profile and core mass of the planet. Here we report on a selection of interior models based on ab initio computer simulations of hydrogen-helium mixtures. We demonstrate that a dilute core, expanded to a significant fraction of the planet's radius, is helpful in reconciling the calculated J(n) with Juno's observations. Although model predictions are strongly affected by the chosen equation of state, the prediction of an enrichment of Z in the deep, metallic envelope over that in the shallow, molecular envelope holds. We estimate Jupiter's core to contain a 7-25 Earth mass of heavy elements. We discuss the current difficulties in reconciling measured J(n) with the equations of state and with theory for formation and evolution of the planet. Plain Language Summary The Juno spacecraft has measured Jupiter's gravity to unprecedented precision. We present models of the planet's interior structure, which treat the hydrogen-helium mixture using computer simulations of the material. We demonstrate that dilute core, with the heavy elements dissolved in hydrogen and expanded outward through a portion of the planet, may be helpful for explaining Juno's measurements.

The Jupiter Inlet I site is situated between the Atlantic coast and the Loxahatchee River in southeast Florida. Although excavations were previously conducted, faunal remains were not systematically collected until recently. Molluscan remains recovered in 2010 are examined to reconstruct past ecological habitats, identify which water bodies were used for extracting resources, and document changes in molluscan species over time. Based upon identifications, only brackish and marine species are represented, indicating that the Loxahatchee River was brackish rather than freshwater during the time of occupation and that the site inhabitants were collecting mollusks from both the lagoon and coastal waters. / Includes bibliography. / Thesis (M.A.)--Florida Atlantic University, 2016. / FAU Electronic Theses and Dissertations Collection

This dissertation combines several new observations of the Io sodium cloud to create a consistent picture of the extended Io atmosphere and its interaction with the Jovian plasma torus. I used the LPL echelle spectrograph to obtain three types of high-resolution spectra of the extended sodium cloud at the sodium D-lines (5890, 5896Å). The first class of observations made use of the mutual satellite eclipses of 1985 to probe the density profile of the atmosphere in the range 1.4 to 10 Io radii, a previously unstudied region. The second type of observation examined the sodium emission in Io's immediate vicinity, allowing an accurate measurement of the velocity structure around Io. The final method employed a high-sensitivity detector to study faint jets of high-speed sodium farther out in the extended cloud. The synthesis of these three data sets results in a better understanding of how sodium is distributed about Io as a function of position and velocity. Io's extended atmosphere is composed of many kinematically distinct components. The distribution in space is linked to their characteristic velocities, with low-energy sodium confined near Io and faster atoms (10 to 100 km sec⁻¹) prevalent beyond ∼25 Io radii. The sodium density profile is steep near Io and shallower outside 5.6 Io radii, the effective limit of Io's gravity. The data indicate that the atmosphere is collisionally thick near the surface, but becomes thin by an altitude of ∼700 km. The upper limit of the exobase location is derived from reliable sodium density measurements made during the satellite eclipses. The lower limit is indirectly inferred from the velocity distribution of sodium near Io and the nature of high-speed jets far from Io. The high-speed sodium jets reveal a new type of close interaction between the corotating plasma and Io's atmosphere. The morphology and brightness of the jets require a two-reaction process, in which atmospheric sodium is ionized, accelerated to high speeds, and then charge-exchanges with other sodium atoms. These processes must occur near the atmospheric exobase, indicating that Io's atmosphere is not completely protected from the plasma flow.