A fundamental approach to phase noise reduction in hybrid Si/III-V lasers

Spontaneous emission into the lasing mode fundamentally limits laser linewidths. Reducing cavity losses provides two benefits to linewidth: (1) fewer excited carriers are needed to reach threshold, resulting in less phase-corrupting spontaneous emission into the laser mode, and (2) more photons are stored in the laser cavity, such that each individual spontaneous emission event disturbs the phase of the field less. Strong optical absorption in III-V materials causes high losses, preventing currently-available semiconductor lasers from achieving ultra-narrow linewidths. This absorption is a natural consequence of the compromise between efficient electrical and efficient optical performance in a semiconductor laser. Some of the III-V layers must be heavily doped in order to funnel excited carriers into the active region, which has the side effect of making the material strongly absorbing.

This thesis presents a new technique, called modal engineering, to remove modal energy from the lossy region and store it in an adjacent low-loss material, thereby reducing overall optical absorption. A quantum mechanical analysis of modal engineering shows that modal gain and spontaneous emission rate into the laser mode are both proportional to the normalized intensity of that mode at the active region. If optical absorption near the active region dominates the total losses of the laser cavity, shifting modal energy from the lossy region to the low-loss region will reduce modal gain, total loss, and the spontaneous emission rate into the mode by the same factor, so that linewidth decreases while the threshold inversion remains constant. The total spontaneous emission rate into all other modes is unchanged.

Modal engineering is demonstrated using the Si/III-V platform, in which light is generated in the III-V material and stored in the low-loss silicon material. The silicon is patterned as a high-Q resonator to minimize all sources of loss. Fabricated lasers employing modal engineering to concentrate light in silicon demonstrate linewidths at least 5 times smaller than lasers without modal engineering at the same pump level above threshold, while maintaining the same thresholds.

The Madden-Julian Oscillation : observation, modeling, and theory

The Madden-Julian Oscillation (MJO) is a pattern of intense rainfall and associated planetary-scale circulations in the tropical atmosphere, with a recurrence interval of 30-90 days. Although the MJO was first discovered 40 years ago, it is still a challenge to simulate the MJO in general circulation models (GCMs), and even with simple models it is difficult to agree on the basic mechanisms. This deficiency is mainly due to our poor understanding of moist convection—deep cumulus clouds and thunderstorms, which occur at scales that are smaller than the resolution elements of the GCMs. Moist convection is the most important mechanism for transporting energy from the ocean to the atmosphere. Success in simulating the MJO will improve our understanding of moist convection and thereby improve weather and climate forecasting.

We address this fundamental subject by analyzing observational datasets, constructing a hierarchy of numerical models, and developing theories. Parameters of the models are taken from observation, and the simulated MJO fits the data without further adjustments. The major findings include: 1) the MJO may be an ensemble of convection events linked together by small-scale high-frequency inertia-gravity waves; 2) the eastward propagation of the MJO is determined by the difference between the eastward and westward phase speeds of the waves; 3) the planetary scale of the MJO is the length over which temperature anomalies can be effectively smoothed by gravity waves; 4) the strength of the MJO increases with the typical strength of convection, which increases in a warming climate; 5) the horizontal scale of the MJO increases with the spatial frequency of convection; and 6) triggered convection, where potential energy accumulates until a threshold is reached, is important in simulating the MJO. Our findings challenge previous paradigms, which consider the MJO as a large-scale mode, and point to ways for improving the climate models.

Magnetic alignment of high-aspect ratio microwires into vertical arrays

Fundamental studies of magnetic alignment of highly anisotropic mesostructures can enable the clean-room-free fabrication of flexible, array-based solar and electronic devices, in which preferential orientation of nano- or microwire-type objects is desired. In this study, ensembles of 100 micron long Si microwires with ferromagnetic Ni and Co coatings are oriented vertically in the presence of magnetic fields. The degree of vertical alignment and threshold field strength depend on geometric factors, such as microwire length and ferromagnetic coating thickness, as well as interfacial interactions, which are modulated by varying solvent and substrate surface chemistry. Microwire ensembles with vertical alignment over 97% within 10 degrees of normal, as measured by X-ray diffraction, are achieved over square cm scale areas and set into flexible polymer films. A force balance model has been developed as a predictive tool for magnetic alignment, incorporating magnetic torque and empirically derived surface adhesion parameters. As supported by these calculations, microwires are shown to detach from the surface and align vertically in the presence of magnetic fields on the order of 100 gauss. Microwires aligned in this manner are set into a polydimethylsiloxane film where they retain their vertical alignment after the field has been removed and can subsequently be used as a flexible solar absorber layer. Finally, these microwires arrays can be protected for use in electrochemical cells by the conformal deposition of a graphene layer.

Understanding planet formation through high precision photometry and spectroscopy

From studies of protoplanetary disks to extrasolar planets and planetary debris, we aim to understand the full evolution of a planetary system. Observational constraints from ground- and space-based instrumentation allows us to measure the properties of objects near and far and are central to developing this understanding. We present here three observational campaigns that, when combined with theoretical models, reveal characteristics of different stages and remnants of planet formation. The Kuiper Belt provides evidence of chemical and dynamical activity that reveals clues to its primordial environment and subsequent evolution. Large samples of this population can only be assembled at optical wavelengths, with thermal measurements at infrared and sub-mm wavelengths currently available for only the largest and closest bodies. We measure the size and shape of one particular object precisely here, in hopes of better understanding its unique dynamical history and layered composition.

Molecular organic chemistry is one of the most fundamental and widespread facets of the universe, and plays a key role in planet formation. A host of carbon-containing molecules vibrationally emit in the near-infrared when excited by warm gas, T~1000 K. The NIRSPEC instrument at the W.M. Keck Observatory is uniquely configured to study large ranges of this wavelength region at high spectral resolution. Using this facility we present studies of warm CO gas in protoplanetary disks, with a new code for precise excitation modeling. A parameterized suite of models demonstrates the abilities of the code and matches observational constraints such as line strength and shape. We use the models to probe various disk parameters as well, which are easily extensible to others with known disk emission spectra such as water, carbon dioxide, acetylene, and hydrogen cyanide.

Lastly, the existence of molecules in extrasolar planets can also be studied with NIRSPEC and reveals a great deal about the evolution of the protoplanetary gas. The species we observe in protoplanetary disks are also often present in exoplanet atmospheres, and are abundant in Earth's atmosphere as well. Thus, a sophisticated telluric removal code is necessary to analyze these high dynamic range, high-resolution spectra. We present observations of a hot Jupiter, revealing water in its atmosphere and demonstrating a new technique for exoplanet mass determination and atmospheric characterization. We will also be applying this atmospheric removal code to the aforementioned disk observations, to improve our data analysis and probe less abundant species. Guiding models using observations is the only way to develop an accurate understanding of the timescales and processes involved. The futures of the modeling and of the observations are bright, and the end goal of realizing a unified model of planet formation will require both theory and data, from a diverse collection of sources.

O argumento pragmático ou consequencialista de cunho econômico e a modulação temporal dos efeitos das decisões do Supremo Tribunal Federal em matéria tributária

A tese analisa a relação íntima que há entre o pragmatismo ou o conseqüencialismo e a modulação temporal dos efeitos das decisões judiciais. Nesta relação, interessa ressaltar o ponto de interseção que certamente sobressai em várias ocasiões: o argumento de cunho econômico. Tal tipo de argumento pode assumir especial relevo quando do exame da oportunidade e conveniência na tomada das decisões eminentemente políticas. No âmbito jurisdicional, no entanto, o argumento pragmático ou consequencialista de cunho econômico não deve prevalecer como fundamento das decisões judiciais, especialmente cuidando-se de matéria tributária. Os problemas que centralizam o estudo podem ser colocados através das seguintes indagações: é possível que o Supremo Tribunal Federal compute, no julgamento de certa matéria tributária, argumento como o eventual rombo de X bilhões de reais que a decisão contrária ao Fisco possa acarretar para os cofres públicos? A fundamentação de eventual decisão judicial calcada exclusiva ou predominantemente em tal argumento é legítima ou ilegítima? Que importância pode ter na tomada de decisão judicial? Quando aplicada, há parâmetros a serem seguidos? Quais? Demonstramos que a prevalência de tal argumento é inadequada na seara judicial, ou seja, deve ter peso reduzido ou periférico, servindo para corroborar ou reforçar os argumentos jurídicos que centralizam o debate submetido ao exame do Poder Judiciário de modo geral, e do Supremo Tribunal Federal, de maneira particular. Em busca de esclarecer quais os principais limites e possibilidades de tal argumento, especialmente relacionando-o à modulação temporal dos efeitos da decisão judicial, explicitamos algumas regras necessárias para a sua adequada utilização, sob pena de inconcebível subversão de variados princípios e direitos fundamentais assegurados em sede constitucional. No exame das questões submetidas à apreciação da Corte Suprema em matéria tributária, o seu parâmetro consiste na maior efetividade e concretude ao texto constitucional. A modulação temporal dos efeitos se aplica a uma decisão que, declarando a inconstitucionalidade do ato normativo, se afastaria ainda mais da vontade constitucional, caso fosse aplicado o tradicional efeito ex tunc (retroativo até o nascimento da lei). Nestas situações específicas e excepcionais se justifica aplicar a modulação, com vistas a dar maior concretude e emprestar maior eficácia à Constituição. A tese proposta, ao final, consiste na reunião das regras explicitadas no trabalho e em proposta legislativa.

A obrigação de extraditar para a repressão do terrorismo: a prática brasileira à luz do direito penal transnacional

O combate efetivo ao flagelo secular do terrorismo, ainda que possa se revestir de muitas formas, não prescinde da repressão penal de seus autores. Em vista da maciça internacionalização do terrorismo, a partir do Século XX, a cooperação jurídica internacional em matéria penal (aí incluída a extradição) consolida-se como instrumento de essencial importância para a repressão do terrorismo pela comunidade internacional, com a vantagem de resguardar o domínio do direito e, por conseguinte, de assegurar a paz e a segurança internacionais. A evolução do tratamento do crime de terrorismo pelo direito penal transnacional influenciada pelo direito da segurança coletiva, especialmente a partir dos atentados de 11 de setembro de 2001 exerceu expressivo impacto no direito extradicional. O entendimento desse efeito é fundamental para extrair-se do instituto da extradição todo o seu potencial para a repressão penal do terrorismo. Desde que presentes determinados requisitos, uma conduta de caráter terrorista à luz de parâmetros internacionais gera a obrigação estatal de extraditar ou processar seu autor, mesmo na ausência de tratado. Além disso, a extradição exercida ou não em decorrência de obrigação convencional tem seus princípios afetados pela obrigação internacional de repressão do terrorismo, particularmente no que se refere a questões como extraditabilidade, extradição por crimes políticos e extradição de refugiados. O direito brasileiro apresenta algumas vulnerabilidades para o cumprimento da obrigação aut dedere aut iudicare e a prática judicial brasileira relativa à extradição de acusados de atos de terrorismo poderia reportar-se mais ao direito internacional, com vistas a evitar o risco de violação de obrigações internacionais pelo Brasil.

I. The effects of variations in certain parameters upon the efficiency of in vivo hemodialysis with a Kiil dialyzer. II. Interfacial structure of concurrent air-water flow in a two-inch diameter horizontal tube.

Part I

Regression analyses are performed on in vivo hemodialysis data for the transfer of creatinine, urea, uric acid and inorganic phosphate to determine the effects of variations in certain parameters on the efficiency of dialysis with a Kiil dialyzer. In calculating the mass transfer rates across the membrane, the effects of cell-plasma mass transfer kinetics are considered. The concept of the effective permeability coefficient for the red cell membrane is introduced to account for these effects. A discussion of the consequences of neglecting cell-plasma kinetics, as has been done to date in the literature, is presented.

A physical model for the Kiil dialyzer is presented in order to calculate the available membrane area for mass transfer, the linear blood and dialysate velocities, and other variables. The equations used to determine the independent variables of the regression analyses are presented. The potential dependent variables in the analyses are discussed.

Regression analyses were carried out considering overall mass-transfer coefficients, dialysances, relative dialysances, and relative permeabilities for each substance as the dependent variables. The independent variables were linear blood velocity, linear dialysate velocity, the pressure difference across the membrane, the elapsed time of dialysis, the blood hematocrit, and the arterial plasma concentrations of each substance transferred. The resulting correlations are tabulated, presented graphically, and discussed. The implications of these correlations are discussed from the viewpoint of a research investigator and from the viewpoint of patient treatment.

Recommendations for further experimental work are presented.

Part II

The interfacial structure of concurrent air-water flow in a two-inch diameter horizontal tube in the wavy flow regime has been measured using resistance wave gages. The median water depth, r.m.s. wave height, wave frequency, extrema frequency, and wave velocity have been measured as functions of air and water flow rates. Reynolds numbers, Froude numbers, Weber numbers, and bulk velocities for each phase may be calculated from these measurements. No theory for wave formation and propagation available in the literature was sufficient to describe these results.

The water surface level distribution generally is not adequately represented as a stationary Gaussian process. Five types of deviation from the Gaussian process function were noted in this work. The presence of the tube walls and the relatively large interfacial shear stresses precludes the use of simple statistical analyses to describe the interfacial structure. A detailed study of the behavior of individual fluid elements near the interface may be necessary to describe adequately wavy two-phase flow in systems similar to the one used in this work.

Bihotz-biriketako berpizte masajeak EKG-an eta bular-inpedantzian eragindako interferentziaren azterketa

[EU]Proiektu honetan bihotz-biriketako berpizte masajearen bular-sakadek elektrokardiograman eta bular-inpedantziaren seinaleetan eragindako interferentziaren azterketa egiten da. Helburu nagusia bi interferentzia hauen arteko erlazioa aztertzea da, horretarako tresna garatuz. Erlazio hau definitzeak interferentziaren eragina txikitzeko modua aurkitzen lagunduko luke, eta honek berpizteko aukerak handituko lituzke. Proiektua gauzatzeko ospitalez kanpoko geldialdien erregistro multzo batetik abiatuta datu-base propioa garatu da ezarritako irizpide batzuk jarraituz. Datu-base berri hau 37 pazienteren 237 mozketak osatzen dute, 10 segundotako luzera minimoarekin non pazienteek asistolia bitarteko kanpoko bular masajea jasotzen duten. Bestalde, interferentzia ezaugarritzeko interfaze grafiko bat garatu da, elektrokardiograma eta bular-inpedantziaren seinaleak denboran eta maiztasunean erakutsi eta hauen parametro esanguratsuak automatikoki zein eskuz ateratzeko aukera ematen duena. Parametroak seinaleen sakada bakoitzeko maximo eta minimoak, beraien kokapenak eta oinarrizko maiztasuna, bere harmonikoak eta hauen anplitudeak dira. Tresna hau erabiliz aipatutako datu-baseko episodioen prozesaketa egin da. Bukatzeko, lortutako emaitzak tratatzeko bigarren interfaze grafiko bat garatu da, non emaitzen banaketa estatistikoa eta hauen arteko erlazio lineala aztertzen diren. Proiektuaren ekarpen nagusia, beraz, bihotz-biriketako berpizte masajeak eragindako interferentzia aztertzeko tresna ahaltsuaren garapena da, jatorri desberdineko bestelako berpizte episodioak aztertzeko ere balio duena.

New Insights from Aperiodic Variability of Young Stars

Nearly all young stars are variable, with the variability traditionally divided into two classes: periodic variables and aperiodic or "irregular" variables. Periodic variables have been studied extensively, typically using periodograms, while aperiodic variables have received much less attention due to a lack of standard statistical tools. However, aperiodic variability can serve as a powerful probe of young star accretion physics and inner circumstellar disk structure. For my dissertation, I analyzed data from a large-scale, long-term survey of the nearby North America Nebula complex, using Palomar Transient Factory photometric time series collected on a nightly or every few night cadence over several years. This survey is the most thorough exploration of variability in a sample of thousands of young stars over time baselines of days to years, revealing a rich array of lightcurve shapes, amplitudes, and timescales.

I have constrained the timescale distribution of all young variables, periodic and aperiodic, on timescales from less than a day to ~100 days. I have shown that the distribution of timescales for aperiodic variables peaks at a few days, with relatively few (~15%) sources dominated by variability on tens of days or longer. My constraints on aperiodic timescale distributions are based on two new tools, magnitude- vs. time-difference (Δm-Δt) plots and peak-finding plots, for describing aperiodic lightcurves; this thesis provides simulations of their performance and presents recommendations on how to apply them to aperiodic signals in other time series data sets. In addition, I have measured the error introduced into colors or SEDs from combining photometry of variable sources taken at different epochs. These are the first quantitative results to be presented on the distributions in amplitude and time scale for young aperiodic variables, particularly those varying on timescales of weeks to months.

Analyses of planetary atmospheres across the spectrum : from Titan to exoplanets

Planetary atmospheres exist in a seemingly endless variety of physical and chemical environments. There are an equally diverse number of methods by which we can study and characterize atmospheric composition. In order to better understand the fundamental chemistry and physical processes underlying all planetary atmospheres, my research of the past four years has focused on two distinct topics. First, I focused on the data analysis and spectral retrieval of observations obtained by the Ultraviolet Imaging Spectrograph (UVIS) instrument onboard the Cassini spacecraft while in orbit around Saturn. These observations consisted of stellar occultation measurements of Titan's upper atmosphere, probing the chemical composition in the region 300 to 1500 km above Titan's surface. I examined the relative abundances of Titan's two most prevalent chemical species, nitrogen and methane. I also focused on the aerosols that are formed through chemistry involving these two major species, and determined the vertical profiles of aerosol particles as a function of time and latitude. Moving beyond our own solar system, my second topic of investigation involved analysis of infra-red light curves from the Spitzer space telescope, obtained as it measured the light from stars hosting planets of their own. I focused on both transit and eclipse modeling during Spitzer data reduction and analysis. In my initial work, I utilized the data to search for transits of planets a few Earth masses in size. In more recent research, I analyzed secondary eclipses of three exoplanets and constrained the range of possible temperatures and compositions of their atmospheres.

Volatiles in Protoplanetary Disks

Planets are assembled from the gas, dust, and ice in the accretion disks that encircle young stars. Ices of chemical compounds with low condensation temperatures (<200 K), the so-called volatiles, dominate the solid mass reservoir from which planetesimals are formed and are thus available to build the protoplanetary cores of gas/ice giant planets. It has long been thought that the regions near the condensation fronts of volatiles are preferential birth sites of planets. Moreover, the main volatiles in disks are also the main C-and O-containing species in (exo)planetary atmospheres. Understanding the distribution of volatiles in disks and their role in planet-formation processes is therefore of great interest.

This thesis addresses two fundamental questions concerning the nature of volatiles in planet-forming disks: (1) how are volatiles distributed throughout a disk, and (2) how can we use volatiles to probe planet-forming processes in disks? We tackle the first question in two complementary ways. We have developed a novel super-resolution method to constrain the radial distribution of volatiles throughout a disk by combining multi-wavelength spectra. Thanks to the ordered velocity and temperature profiles in disks, we find that detailed constraints can be derived even with spatially and spectrally unresolved data -- provided a wide range of energy levels are sampled. We also employ high-spatial resolution interferometric images at (sub)mm frequencies using the Atacama Large Millimeter Array (ALMA) to directly measure the radial distribution of volatiles.

For the second question, we combine volatile gas emission measurements with those of the dust continuum emission or extinction to understand dust growth mechanisms in disks and disk instabilities at planet-forming distances from the central star. Our observations and models support the idea that the water vapor can be concentrated in regions near its condensation front at certain evolutionary stages in the lifetime of protoplanetary disks, and that fast pebble growth is likely to occur near the condensation fronts of various volatile species.

Mercados financieros: análisis fundamental y técnico

Explicación de conceptos claves relacionados con los mercados financieros desde una perspectiva simple y dirigida a personas sin grandes conocimientos de la materia.

Fundamental aspects of the feeding of the amphipod Gammarus (R.) balcanicus (Crustacea, Amphipoda). [Translation from: Nauchn.Dokl.vyssh.Shkoly (Biol.Nauk) 1970(7) 12-16, 1970]

The amphipods are major food items for many commercial fishes, and they are used as protein food for agricultural animals. In the present paper are presented the results of four-year observations on the feeding of Gammarus balcanicus in nature and in an aquarium. Among the studied aspects were the dependence of daily food ration on sex and physiological state (with and without eggs) and feeding on different kinds of plant food. The study concludes that Gammarus balcanicus willingly feed on soft half-decayed plant residues; into their ration also enters food of animal origin. In contrast to other amphipods, G. balcanicus eats representatives of its own species very rarely, and only dead or immobile ones.