Rotação diferencial em estrelas do tipo solar

Stellar differential rotation is an important key to understand hydromagnetic stellar dynamos, instabilities, and transport processes in stellar interiors as well as for a better treatment of tides in close binary and star-planet systems. The space-borne high-precision photometry with MOST, CoRoT, and Kepler has provided large and homogeneous datasets. This allows, for the first time, the study of differential rotation statistically robust samples covering almost all stages of stellar evolution. In this sense, we introduce a method to measure a lower limit to the amplitude of surface differential rotation from high-precision evenly sampled photometric time series such as those obtained by space-borne telescopes. It is designed for application to main-sequence late-type stars whose optical flux modulation is dominated by starspots. An autocorrelation of the time series is used to select stars that allow an accurate determination of spot rotation periods. A simple two-spot model is applied together with a Bayesian Information Criterion to preliminarily select intervals of the time series showing evidence of differential rotation with starspots of almost constant area. Finally, the significance of the differential rotation detection and a measurement of its amplitude and uncertainty are obtained by an a posteriori Bayesian analysis based on a Monte Carlo Markov Chain (hereafter MCMC) approach. We apply our method to the Sun and eight other stars for which previous spot modelling has been performed to compare our results with previous ones. The selected stars are of spectral type F, G and K. Among the main results of this work, We find that autocorrelation is a simple method for selecting stars with a coherent rotational signal that is a prerequisite to a successful measurement of differential rotation through spot modelling. For a proper MCMC analysis, it is necessary to take into account the strong correlations among different parameters that exists in spot modelling. For the planethosting star Kepler-30, we derive a lower limit to the relative amplitude of the differential rotation. We confirm that the Sun as a star in the optical passband is not suitable for a measurement of the differential rotation owing to the rapid evolution of its photospheric active regions. In general, our method performs well in comparison with more sophisticated procedures used until now in the study of stellar differential rotation

Comparison between Two Methods to Calculate the Transition Matrix of Orbit Motion

Two methods to evaluate the state transition matrix are implemented and analyzed to verify the computational cost and the accuracy of both methods. This evaluation represents one of the highest computational costs on the artificial satellite orbit determination task. The first method is an approximation of the Keplerian motion, providing an analytical solution which is then calculated numerically by solving Kepler's equation. The second one is a local numerical approximation that includes the effect of J(2). The analysis is performed comparing these two methods with a reference generated by a numerical integrator. For small intervals of time (1 to 10s) and when one needs more accuracy, it is recommended to use the second method, since the CPU time does not excessively overload the computer during the orbit determination procedure. For larger intervals of time and when one expects more stability on the calculation, it is recommended to use the first method.

Fatores do ambiente sobre o peso ao desmame de bezerros da raça nelore em regiões tropicais brasileiras

Este trabalho teve o objetivo de estudar a influência de efeitos não genéticos sobre o peso ao desmame de 105.465 bezerros da raça Nelore, nascidos em oito diferentes regiões brasileiras, no período de 1978 a 1994. A análise estatística foi realizada utilizando-se o método dos quadrados mínimos, procedimento GLM (SAS, 1996), com um modelo estatístico contendo como fontes de variação os efeitos fixos de sexo, mês e ano de nascimento do bezerro, região, fazenda dentro de região, grupo de idade da vaca e, como efeitos aleatórios, touro e o erro. Todas as fontes de variação do modelo foram significativas (P<0,0001). A importância desses efeitos não genéticos sobre o peso aos 205 dias de idade de bezerros da raça Nelore evidenciam a necessidade de se fazer ajustes para os mesmos, visto que estes influenciaram sobre a característica estudada.

Spin-orbit coupling for tidally evolving super-Earths

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

Da geografia medieval às origens da geografia moderna: contrastes entre diferentes noções de natureza, espaço e tempo

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Cálculo diferencial e integral no movimento dos planetas

Pós-graduação em Matemática em Rede Nacional - IBILCE

The spin-orbit resonant problem including core-mantle gravitational coupling

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

Ressonâncias planetárias spin-órbita com perturbação de terceiro corpo

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

Dynamics of the 3:1 resonant planetary systems

Many of the discovered exoplanetary systems are involved inside mean-motion resonances. In this work we focus on the dynamics of the 3:1 mean-motion resonant planetary systems. Our main purpose is to understand the dynamics in the vicinity of the apsidal corotation resonance (ACR) which are stationary solutions of the resonant problem. We apply the semi-analytical method (Michtchenko et al., 2006) to construct the averaged three-body Hamiltonian of a planetary system near a 3:1 resonance. Then we obtain the families of ACR, composed of symmetric and asymmetric solutions. Using the symmetric stable solutions we observe the law of structures (Ferraz-Mello,1988), for different mass ratio of the planets. We also study the evolution of the frequencies of σ1, resonant angle, and Δω, the secular angle. The resonant domains outside the immediate vicinity of ACR are studied using dynamical maps techniques. We compared the results obtained to planetary systems near a 3:1 MMR, namely 55 Cnc b-c, HD 60532 b-c and Kepler 20 b-c.

PLANEJAMENTO, OBJETIVOS E DEFINIÇÃO DE PADRÕES NA DESCRIÇÃO DOS METADADOS DA COLEÇÃO DA BIBLIOTECA BRASILIANA DIGITAL

O projeto „Por uma Biblioteca Brasiliana Digital‟ é parte integrante do projeto BRASILIANA USP, uma iniciativa da Reitoria da Universidade de São Paulo (USP), que tem por objetivo facultar para a pesquisa a maior Brasiliana custodiada por uma universidade, tornando-a disponível na internet. O trabalho que ora apresentamos é resultado da implantação de um modelo de biblioteca digital que atende aos padrões de interoperabilidade e compartilhamento de informações. Especificamente, apresentaremos os procedimentos e processos de descrição de conteúdos das diversas tipologias documentais (livros, periódicos, mapas, gravuras etc.) e formatos digitais (pdf, mp3, jpeg entre outros), bem como a consolidação de um esquema de metadados gerenciais e administrativos que contemplam as informações e dados produzidos pelo Projeto da Brasiliana Digital.

Keplero e la musica. Il Libro III dell'Harmonice mundi (Linz, 1619): traduzione e Introduzione

Questo lavoro si concentra su un particolare aspetto della sfaccettata ricerca scientifica di Johannes Kepler (1571-1630), ossia quello teorico-musicale. I pensieri dell’astronomo tedesco riguardanti tale campo sono concentrati – oltre che in alcuni capitoli del Mysterium cosmographicum (1596) ed in alcune sue lettere – nel Libro III dell’Harmonices mundi libri quinque (1619), che, per la sua posizione mediana all’interno dell’opera, tra i primi due libri geometrici e gli ultimi due astronomici, e per la sua funzione di raccordo tra la «speculazione astratta» della geometria e la concretizzazione degli archetipi geometrici nel mondo fisico, assume la struttura di un vero e proprio trattato musicale sul modello di quelli rinascimentali, nel quale la «musica speculativa», dedicata alla teoria delle consonanze e alla loro deduzione geometrica precede la «musica activa», dedicata alla pratica del canto dell’uomo nelle sue differenze, generi e modi. La tesi contiene la traduzione italiana, con testo latino a fronte, del Libro III dell’Harmonice, e un’ampia introduzione che percorre le tappe fondamentali del percorso biografico e scientifico che hanno portato alla concezione di quest’opera – soffermandosi in particolare sulla formazione musicale ricevuta da Keplero, sulle pagine di argomento musicale del Mysterium e delle lettere, e sulle riflessioni filosofico-armoniche sviluppate negli anni di ricerca – e offre gli elementi fondamentali per poter comprendere l’Harmonice mundi in generale e il Libro III in particolare. A ciò si aggiunge, in Appendice, la traduzione, anch’essa con testo latino a fronte, della Sectio V, dedicata alla musica, del Liber IX dell’Almagestum novum (1651) di Giovanni Battista Riccioli (1598-1671), interessante sia dal punto di vista della recezione delle teorie di Keplero che dal punto di vista della storia delle idee musicali.

Validität und Reliabilität bei der visuellen okklusalen Kariesdiagnostik mit ICDAS unter der Verwendung von unterschiedlichen dentalen Vergrösserungshilfen

Zielsetzung: Diese Studie untersuchte die Validität und Reliabilität von verschiedenen visuellen dentalen Vergrösserungshilfen in Bezug auf die okklusale Kariesdiagnostik mit Hilfe des International Caries Detection and Assessment System (ICDAS). Material und Methode: Die Okklusalflächen von 100 extrahierten Zähnen wurde an einer zuvor bestimmten Stelle von 10 Studenten (5 Studenten des 3. Jahreskurses (Bachelor-Studenten) und 5 Studenten des 4. Jahreskurses (Master-Studenten) der Zahnmedizinischen Kliniken der Universität Bern) und 4 Zahnärzten visuell untersucht und nach ICDAS auf das Vorhandensein und die Tiefe einer kariösen Läsion beurteilt. Die Beurteilung der Zähne erfolgte je zwei Mal von blossem Auge, mit einem Galilei-Lupensystem (2.5x Vergrösserung), mit einem Kepler-Lupensystem (4.5x Vergrösserung) und mit dem Operationsmikroskop (10x Vergrösserung) mit mindestens 24 Stunden Abstand zwischen den jeweiligen Untersuchungen. Als Goldstandard diente die Histologie. Die statistische Auswertung der Untersuchungen erfolgte mit der Berechnung der Kappa-Koeffizienten für die Intra- und Inter-Untersucher Reliabilität sowie einer Bayes-Analyse durch Ermittlung von Sensitivität, Spezifität und der Fläche unter der Receiver Operating Characteristic Kurve (AUC). Ergebnisse: Bei den Untersuchungsdurchläufen, welche mit dentalen Vergrösserungshilfen für die Diagnostik der okklusalen Zahnoberflächen durchgeführt wurden, sank die Anzahl der mit einem ICDAS-Code 0 (gesunde Zahnoberfläche) beurteilten Zähne, während die Quantität des Codes 3 (Schmelzeinbruch) mit höheren Vergrösserungen drastisch zunahm. Mit steigendem Vergrösserungsfaktor liessen sich sowohl mehr Schmelzkaries als auch Dentinkaries richtig erkennen (bessere Sensitivität), im Gegenzug sanken aber die Werte der Spezifität auf ein klinisch unakzeptables Niveau. Während der Abfall der Spezifität und AUC-Werte bei der Beurteilung von Schmelzkaries unter Verwendung von kleinen Vergrösserungen lediglich einen Trend darstellte, waren die Verschlechterungen in der Diagnostik bei der Dentinkaries unter der Zuhilfenahme von höheren Vergrösserungen häufig signifikant. So stiegen zum Beispiel bei den Zahnärzten die Werte der Sensitivität (Bandbreite) auf dem D3-Diagnostikniveau von 0.47 (0.17-0.79) bei dem Durchlauf von Auge auf 0.91 (0.83-1.00) bei der Benutzung des Operationsmikroskopes an, während jedoch die Spezifitätswerte (Bandbreite) von 0.78 (0.58-0.95) auf 0.30 (0.07-0.55) sanken. Ebenfalls einen negativen Einfluss von optischen Hilfsmitteln zeigte sich bei der Inter-Untersucher Reliabilität, während die Intra-Untersucher Reliabilität unbeeinflusst blieb. Die persönliche klinische Erfahrung scheint sowohl in Bezug auf das Mass der Übereinstimmung visueller Kariesdiagnostik als auch auf die Präferenz bei der Vergabe der ICDAS-Codes und somit auf die Werte der Validität einen wesentlichen Faktor auszumachen. Die Studenten erreichten die besten Werte der Sensitivität, indes die Zahnärzte dies bei der Spezifität erzielten. Schlussfolgerung: Insgesamt zeigte sich, dass ICDAS nicht für den zusätzlichen Gebrauch von optischen Vergrösserungen konzipiert wurde. Da es auf Grund von der Zuhilfenahme von dentalen Vergrösserungen zu mehr und unnötigen invasiven Behandlungsentscheidungen kommen könnte, ist von der Zuhilfenahme derselben für die okklusale Kariesdiagnostik mit ICDAS abzuraten.

UNDERSTANDING TRENDS ASSOCIATED WITH CLOUDS IN IRRADIATED EXOPLANETS

Unlike previously explored relationships between the properties of hot Jovian atmospheres, the geometric albedo and the incident stellar flux do not exhibit a clear correlation, as revealed by our re-analysis of Q0-Q14 Kepler data. If the albedo is primarily associated with the presence of clouds in these irradiated atmospheres, a holistic modeling approach needs to relate the following properties: the strength of stellar irradiation (and hence the strength and depth of atmospheric circulation), the geometric albedo (which controls both the fraction of starlight absorbed and the pressure level at which it is predominantly absorbed), and the properties of the embedded cloud particles (which determine the albedo). The anticipated diversity in cloud properties renders any correlation between the geometric albedo and the stellar flux weak and characterized by considerable scatter. In the limit of vertically uniform populations of scatterers and absorbers, we use an analytical model and scaling relations to relate the temperature-pressure profile of an irradiated atmosphere and the photon deposition layer and to estimate whether a cloud particle will be lofted by atmospheric circulation. We derive an analytical formula for computing the albedo spectrum in terms of the cloud properties, which we compare to the measured albedo spectrum of HD 189733b by Evans et al. Furthermore, we show that whether an optical phase curve is flat or sinusoidal depends on whether the particles are small or large as defined by the Knudsen number. This may be an explanation for why Kepler-7b exhibits evidence for the longitudinal variation in abundance of condensates, while Kepler-12b shows no evidence for the presence of condensates despite the incident stellar flux being similar for both exoplanets. We include an "observer's cookbook" for deciphering various scenarios associated with the optical phase curve, the peak offset of the infrared phase curve, and the geometric albedo.