This thesis provides a multi-pronged approach towards paving the way for future space and ground based exoplanet characterisation e↵orts as well as providing new analysis of the atmosphere of the exoplanet HD 179949 b. This is done, firstly, by outlining engineering trade studies conducted for the attitude and orbit control system (AOCS) and sun shield for the Exoplanet Characterisation Observatory (EChO) spacecraft (a proposed European Space Agency exoplanet space mission). These trade studies were conducted in collaboration with EADS Astrium. A cold gas system with the possibility of a hybrid system which would include the use of reaction wheels is recommend for the design of the AOCS. For the sun shield, a V-groove cone shield is concluded to provide the best thermal coverage while also providing stay light protection as well as being more mechanically symmetric than other options. Simulations are then conducted to determine the number of transiting planets future surveys should expect to find around stars within 50 parsecs of the sun. This is done by taking the known stars within 50 parsecs and adding a simulated planet population based on current models and observations to each star. Assumptions are made regarding observability of a planetary transit and a Monte Carlo simulation run to gain statistics on the number and type of planetary systems that can be expected to be found. The results of the simulation show a mean expected number of 27 detectable transiting planets within 50 parsecs. Next, using the Position and Proper Motion Extended-L (PPMXL) catalogue, optical and near-infrared colour cuts were used together with a reduced proper motion cut to find bright M dwarfs for future exoplanet transit studies. PPMXL’s low proper motion uncertainties allow this work to probe down to smaller proper motions than previous similar studies. Unique objects found with this method were combined with that of previous work to produce 8479 K < 9 M dwarfs. Low-resolution spectroscopy was obtained of a sample of the objects found using this selection method to gain statistics on their spectral type and physical properties. Results show a spectral-type range of K7-M4V. This catalogue is the most complete collection of K < 9 M dwarfs currently available and is made available here. High resolution spectroscopy and model spectra of planetary atmospheres is then used along with a spectral deconvolution technique to attempt to detect the Doppler shifted signal of the non-transiting planet HD 179949 b. The signal was not detected but new upper limits were set ruling out the presence of TiO down to a log10 ✏0 = -4.09 with 99.9 per cent confidence. Simulations conducted by this work imply a loss of sensitivity occurring possibly due to varying telluric interference or instrumental systematics.

Este trabalho descreve técnicas de espectroscopia de alta resolução em sólidos por Ressonância Magnética Nuclear (RMN), o projeto de construção de um espectrômetro para este fim e sua avaliação experimental com a utilização deste equipamento na caracterização de amostras sólidas. O espectrômetro de alta resolução em sólidos por RMN desenvolvido, permite a utilização de técnicas de dupla ressonância, múltiplos pulsos e rotação da amostra em tomo do ângulo mágico e pode também ser utilizado para líquidos. A máxima freqüência de rotação para MAS é da ordem de 5KHz e as seqüências de dupla ressonância podem ser utilizadas pala quaisquer pares de núcleos atômicos. Os experimentos podem ser realizados com variação de temperatura de -120&#176C a + 160&#176C e o equipamento é totalmente controlado por um microcomputador Macintosh IIci. / This work describes the nuclear magnetic resonance (NMR) techniques for High Resolution Spectroscopy in Solids. Also, the construction project of a partially \"home made\" spectrometer and its applications in the characterization of solid samples are shown in detail. Our high resolution spectrometer is implemented with the double resonance multiple pulses sequences and magic angle spinning (MAS) and can be used with solid and liquid samples. The maximum spinning frequency for the MAS experiment is in excess of 5KHz, the double resonance sequences can be performed with any type of nucleus, in the variable temperature operating range with nitrogen gas: -120&#176C to +160&#176C, and is fully controlled by a Macintosh IIci microcomputer.

Thesis (Ph.D.)--Massachusetts Institute of Technology, Dept. of Chemistry, 1979. / MICROFICHE COPY AVAILABLE IN ARCHIVES AND SCIENCE. / Includes bibliographical references. / Ph.D.

Este trabalho descreve técnicas de espectroscopia de alta resolução em sólidos por Ressonância Magnética Nuclear (RMN), o projeto de construção de um espectrômetro para este fim e sua avaliação experimental com a utilização deste equipamento na caracterização de amostras sólidas. O espectrômetro de alta resolução em sólidos por RMN desenvolvido, permite a utilização de técnicas de dupla ressonância, múltiplos pulsos e rotação da amostra em tomo do ângulo mágico e pode também ser utilizado para líquidos. A máxima freqüência de rotação para MAS é da ordem de 5KHz e as seqüências de dupla ressonância podem ser utilizadas pala quaisquer pares de núcleos atômicos. Os experimentos podem ser realizados com variação de temperatura de -120&#176C a + 160&#176C e o equipamento é totalmente controlado por um microcomputador Macintosh IIci. / This work describes the nuclear magnetic resonance (NMR) techniques for High Resolution Spectroscopy in Solids. Also, the construction project of a partially \"home made\" spectrometer and its applications in the characterization of solid samples are shown in detail. Our high resolution spectrometer is implemented with the double resonance multiple pulses sequences and magic angle spinning (MAS) and can be used with solid and liquid samples. The maximum spinning frequency for the MAS experiment is in excess of 5KHz, the double resonance sequences can be performed with any type of nucleus, in the variable temperature operating range with nitrogen gas: -120&#176C to +160&#176C, and is fully controlled by a Macintosh IIci microcomputer.

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Thesis (Ph. D.)--Joint Program in Applied Ocean Sciences (Massachusetts Institute of Technology, Dept. of Ocean Engineering; and the Woods Hole Oceanographic Institution), 2002. / Includes bibliographical references (leaves 161-170).

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Herbig Ae/Be (HAeBe) stars are the pre-main sequence progenitors of main sequence A and B stars, and are characterized observationally by strong emission in spectral lines and significant infra-red excess that results from their presence in dust-obscured regions. These stars are usually surrounded by a complex environment composed of gas and dust and often a significant stellar wind and a circumstellar disc. This complex circumstellar environment can have a significant affect on their spectral energy distributions, leading to large systematic uncertainties in determinations of their effective temperatures from photometric methods. In an attempt to improve temperature determinations for HAeBe stars, we have conducted an experiment to evaluate the potential of high-resolution spectra to constrain their atmospheric parameters. To this end, high-resolution (R~68 000) and low-resolution (R~1500) spectra obtained using the ESPaDOnS spectropolarimeter (at the Canada-France-Hawaii telescope) and the FORS1 spectropolarimeter (at the Very Large Telescope) have been used with an automatic spectrum fitting procedure. This procedure compares spectroscopic data to a grid of synthetic LTE, solar abundance spectra, spanning a range in effective temperature, surface gravity, and micro-turbulence. This analysis was applied to the spectra of a sample of twelve previously well-studied HAeBe stars. Our temperatures were found to be consistent with previously published values, while providing much lower uncertainties - in some cases about 5 times smaller. Numerous methods were investigated to obtain these quantitative uncertainties (chi-squared statistics, Bayesian analysis, Monte Carlo bootstrap method, individual temperature sensitive line region analysis). We conclude that our method can be used to efficiently and effectively obtain temperatures of HAeBe stars in addition to providing us with a characterization of the degree of departure of the spectrum from solar abundance, LTE photospheric models. / Thesis (Master, Physics, Engineering Physics and Astronomy) -- Queen's University, 2009-02-13 10:23:04.9

The effect of short, strong radiofrequency pulses on the nuclear spin system is examined. Providing the durations of the pulses are short with respect to coupling constants within the spin system, they may be described by simple rotation operators which are exponential functions of the angular momentum operators. Operator algebra can be used to define the interaction of such pulses with the spin system, and the mutual interaction of a sequence of pulses. The case of a simple coupled spin system is examined in detail and it is found that a vector model can be used to describe the motion of the expectation values of the observables. This model also allows treatment of such 'non-classical 1 effects as coherence transfer and multiple-quantum coherence. The proposal is also made that certain types of pulse imperfection may be compensated by using specially constructed sequences of small numbers of pulses, which are termed 'composite pulses'. Their compensatory action is illustrated by computer simulation, and by experimental results. In the case of certain symmetrical composite pulses, operator algebra can be used to understand their overall effect in the presence of pulse imperfections, suggesting their use in such critical applications as multiple spin echo trains. Another class of symmetrical composite pulses provides rotations by arbitrary angles around the z-axis of the rotating reference frame, and is expected to be of use in multiple-quantum spectroscopy.