Serie Vídeos tutoriales para fonética. Video 6. Praat: doing phonetics by computer (Parte 2: Propiedades acústicas de los sonidos del habla observables en oscilogramas)

Esta es una colección de 10 vídeos tutoriales que pueden ser empleados como material educativo en los cursos de fonética básica en el ámbito universitario. Los vídeos 1-3 tratan aspectos relacionados con la grabación: el tipo de micrófonos que se emplean, las clases de espacios en las que se suelen llevar a cabo la captura de señales de audio y las grabadoras que se suelen emplear. El vídeo 4 explora técnicas de captura y observación de datos de flujo y presión en fonética aerodinámica. Los vídeos 5-10 presentan información sobre los principales usos que se le brindan al programa Praat (Boersma y Weenink, 2014) en los estudios actuales de fonética acústica, desde la clase de información sobre modos de articulación de las consonantes que se puede identificar en oscilogramas hasta la creación de señales sonoras sintetizadas por medio de unos procedimientos que tiene el programa para tal propósito, los cuales son susceptibles de ser empleados en experimentos de percepción auditiva.

Serie Vídeos tutoriales para fonética. Video 10. Praat: doing phonetics by computer (Parte 6: Manipulación y síntesis de señales sonoras)

Esta es una colección de 10 vídeos tutoriales que pueden ser empleados como material educativo en los cursos de fonética básica en el ámbito universitario. Los vídeos 1-3 tratan aspectos relacionados con la grabación: el tipo de micrófonos que se emplean, las clases de espacios en las que se suelen llevar a cabo la captura de señales de audio y las grabadoras que se suelen emplear. El vídeo 4 explora técnicas de captura y observación de datos de flujo y presión en fonética aerodinámica. Los vídeos 5-10 presentan información sobre los principales usos que se le brindan al programa Praat (Boersma y Weenink, 2014) en los estudios actuales de fonética acústica, desde la clase de información sobre modos de articulación de las consonantes que se puede identificar en oscilogramas hasta la creación de señales sonoras sintetizadas por medio de unos procedimientos que tiene el programa para tal propósito, los cuales son susceptibles de ser empleados en experimentos de percepción auditiva.

Synthesis of (±)-7,8-epoxy-4-basmen-6-one by a transannular cyclization strategy

The first synthesis of the cembranoid natural product (±)-7,8-epoxy-4-basmen-6- one (1) is described. Key steps of the synthetic route include the cationic cyclization of the acid chloride from 15 to provide the macrocycle 16, and the photochemical transannular radical cyclization of the ester 41 to form the tricyclic product 50. Product 50 was transformed into 1 in ten steps. Transition-state molecular modeling studies were found to provide accurate predictions of the structural and stereochemical outcomes of cyclization reactions explored experimentally in the development of the synthetic route to 1. These investigations should prove valuable in the development of transannular cyclization as a strategy for synthetic simplification.

1. Astronomical photometry at wavelengths of 8.5, 10.5, and 11.6 µm. 2. Infrared emission from asteroids at wavelengths of 8.5, 10.5, and 11.6 µm

The purpose of this thesis is to present new observations of thermal-infrared radiation from asteroids. Stellar photometry was performed to provide standards for comparison with the asteroid data. The details of the photometry and the data reduction are discussed in Part 1. A system of standard stars is derived for wavelengths of 8.5, 10.5 and 11.6 µm and a new calibration is adopted. Sources of error are evaluated and comparisons are made with the data of other observers.

The observations and analysis of the thermal-emission observations of asteroids are presented in Part 2. Thermal-emission lightcurve and phase effect data are considered. Special color diagrams are introduced to display the observational data. These diagrams are free of any model-dependent assumptions and show that asteroids differ in their surface properties.

On the basis of photometric models, (4) Vesta is thought to have a bolometric Bond albedo of about 0.1, an emissivity greater than 0.7 and a true radius that is close to the model value of 300^(+50)_(-30)km. Model albedos and model radii are given for asteroids 1, 2, 4, 5, 6, 7, 15, 19, 20, 27, 39, 44, 68, 80, 324 and 674. The asteroid (324) Bamberga is extremely dark with a model (~bolometric Bond) albedo in the 0.01 - 0.02 range, which is thought to be the lowest albedo yet measured for any solar-system body. The crucial question about such low-albedo asteroids is their number and the distribution of their orbits.

Observations of 1-6 MeV Jovian electrons at 1 AU and a study of their propagation

The 1-6 MeV electron flux at 1 AU has been measured for the time period October 1972 to December 1977 by the Caltech Electron/Isotope Spectrometers on the IMP-7 and IMP-8 satellites. The non-solar interplanetary electron flux reported here covered parts of five synodic periods. The 88 Jovian increases identified in these five synodic periods were classified by their time profiles. The fall time profiles were consistent with an exponential fall with τ ≈ 4-9 days. The rise time profiles displayed a systematic variation over the synodic period. Exponential rise time profiles with τ ≈ 1-3 days tended to occur in the time period before nominal connection, diffusive profiles predicted by the convection-diffusion model around nominal connection, and abrupt profiles after nominal connection.

The times of enhancements in the magnetic field, │B│, at 1 AU showed a better correlation than corotating interaction regions (CIR's) with Jovian increases and other changes in the electron flux at 1 AU, suggesting that │B│ enhancements indicate the times that barriers to electron propagation pass Earth. Time sequences of the increases and decreases in the electron flux at 1 AU were qualitatively modeled by using the times that CIR's passed Jupiter and the times that │B│ enhancements passed Earth.

The electron data observed at 1 AU were modeled by using a convection-diffusion model of Jovian electron propagation. The synodic envelope formed by the maxima of the Jovian increases was modeled by the envelope formed by the predicted intensities at a time less than that needed to reach equilibrium. Even though the envelope shape calculated in this way was similar to the observed envelope, the required diffusion coefficients were not consistent with a diffusive process.

Three Jovian electron increases at 1 AU for the 1974 synodic period were fit with rise time profiles calculated from the convection-diffusion model. For the fits without an ambient electron background flux, the values for the diffusion coefficients that were consistent with the data were k_x = 1.0 - 2.5 x 10²¹ cm²/sec and k_y = 1.6 - 2.0 x 10²² cm²/sec. For the fits that included the ambient electron background flux, the values for the diffusion coefficients that were consistent with the data were k_x = 0.4 - 1.0 x 10²¹ cm²/sec and k_y = 0.8 - 1.3 x 10²² cm²/sec.

On the nutrition of the predatory cladocerans Leptodora and Bythotrephes. [Translation of: Byulleten' Institute Biologii Vodokhranilishch 6, pp. 21-22, 1960]

Results of the investigation on certain problems of the nutrition of Leptodora and Bythotrephes in Rybinsk Reservoir (Russia) are reviewed. To clarify the composition of the food of Leptodora and Bythotrephes in this period, experiments were provided on their nutrition by cyclopids and rotifers.

On the structure of the seminal receptacle in cyclopids (Copepoda, Cyclopoida). [Translation from: Informatsionnyi Byulleten Biologiya Vnutrennikh Vod (6) 26-31, 1970.]

The seminal bag, or seminal receptacle, forms a characteristic organ of cyclopids, serving for retention of the sperms discharged from the spermatophores. The structure of the seminal receptacle, more precisely its form, is fairly widely used in diagnosis and undoubtedly can be more widely applied in the systematics of the group. Within the limits of the family Cyclopidae it is possible to distinguish crustaceans with three basic types of seminal bag. The differences consist of the position which this organ occupies in the genital segment. of one species, we carried out a series of observations on its formation in ontogenesis and during the life of the adult stage. As material for observation the study used laboratory cultures of three species; Acanthocyclops americanus (Marsh) from the plankton of the Moscow River, Cyclops vicinus Uljan and Mesocyclops leuckarti Glaus from the plankton of the channel section of the upper part of the Gorkovsk reservoir. The author concluded that the irreversibility of the changes in the seminal receptacle presents the possibility of utilising this structure as one of the indicators of the growth of the individual.

Activity of perch, Perca fluviatilis L. in relation to water temperature [Translation from: Kalamies 1973(6) 4.]

Catchability and activity of Perca fluviatilis in relation to temperature is examined. The number of fish caught and water temperature during the 3 summer months was used the assess the numbers of hours of activity of perch. Parallel to the research on activity, large-scale marking was carried out to establish the periods of growth during the year.

Reaction of fish to light (”Conclusions” only). [Translation from: Voprosy Ikhtiologii 6 17-20, 1956]

Qualitative and quantitative characteristics of the reaction of certain fish to light were tested and reasons for the attraction of certain fish to light are discussed.

Toward Understanding Astrophysical Phenomena

Fast radio bursts (FRBs), a novel type of radio pulse, whose physics is not yet understood at all. Only a handful of FRBs had been detected when we started this project. Taking account of the scant observations, we put physical constraints on FRBs. We excluded proposals of a galactic origin for their extraordinarily high dispersion measures (DM), in particular stellar coronas and HII regions. Therefore our work supports an extragalactic origin for FRBs. We show that the resolved scattering tail of FRB 110220 is unlikely to be due to propagation through the intergalactic plasma. Instead the scattering is probably caused by the interstellar medium in the FRB's host galaxy, and indicates that this burst sits in the central region of that galaxy. Pulse durations of order $\ms$ constrain source sizes of FRBs implying enormous brightness temperatures and thus coherent emission. Electric fields near FRBs at cosmological distances would be so strong that they could accelerate free electrons from rest to relativistic energies in a single wave period. When we worked on FRBs, it was unclear whether they were genuine astronomical signals as distinct from `perytons', clearly terrestrial radio bursts, sharing some common properties with FRBs. Recently, in April 2015, astronomers discovered that perytons were emitted by microwave ovens. Radio chirps similar to FRBs were emitted when their doors opened while they were still heating. Evidence for the astronomical nature of FRBs has strengthened since our paper was published. Some bursts have been found to show linear and circular polarizations and Faraday rotation of the linear polarization has also been detected. I hope to resume working on FRBs in the near future. But after we completed our FRB paper, I decided to pause this project because of the lack of observational constraints.

The pulsar triple system, J0733+1715, has its orbital parameters fitted to high accuracy owing to the precise timing of the central $\ms$ pulsar. The two orbits are highly hierarchical, namely $P_{\mathrm{orb,1}}\ll P_{\mathrm{orb,2}}$, where 1 and 2 label the inner and outer white dwarf (WD) companions respectively. Moreover, their orbital planes almost coincide, providing a unique opportunity to study secular interaction associated purely with eccentricity beyond the solar system. Secular interaction only involves effect averaged over many orbits. Thus each companion can be represented by an elliptical wire with its mass distributed inversely proportional to its local orbital speed. Generally there exists a mutual torque, which vanishes only when their apsidal lines are parallel or anti-parallel. To maintain either mode, the eccentricity ratio, $e_1/e_2$, must be of the proper value, so that both apsidal lines precess together. For J0733+1715, $e_1\ll e_2$ for the parallel mode, while $e_1\gg e_2$ for the anti-parallel one. We show that the former precesses $\sim 10$ times slower than the latter. Currently the system is dominated by the parallel mode. Although only a little anti-parallel mode survives, both eccentricities especially $e_1$ oscillate on $\sim 10^3\yr$ timescale. Detectable changes would occur within $\sim 1\yr$. We demonstrate that the anti-parallel mode gets damped $\sim 10^4$ times faster than its parallel brother by any dissipative process diminishing $e_1$. If it is the tidal damping in the inner WD, we proceed to estimate its tidal quantity parameter ($Q$) to be $\sim 10^6$, which was poorly constrained by observations. However, tidal damping may also happen during the preceding low-mass X-ray binary (LMXB) phase or hydrogen thermal nuclear flashes. But, in both cases, the inner companion fills its Roche lobe and probably suffers mass/angular momentum loss, which might cause $e_1$ to grow rather than decay.

Several pairs of solar system satellites occupy mean motion resonances (MMRs). We divide these into two groups according to their proximity to exact resonance. Proximity is measured by the existence of a separatrix in phase space. MMRs between Io-Europa, Europa-Ganymede and Enceladus-Dione are too distant from exact resonance for a separatrix to appear. A separatrix is present only in the phase spaces of the Mimas-Tethys and Titan-Hyperion MMRs and their resonant arguments are the only ones to exhibit substantial librations. When a separatrix is present, tidal damping of eccentricity or inclination excites overstable librations that can lead to passage through resonance on the damping timescale. However, after investigation, we conclude that the librations in the Mimas-Tethys and Titan-Hyperion MMRs are fossils and do not result from overstability.

Rubble piles are common in the solar system. Monolithic elements touch their neighbors in small localized areas. Voids occupy a significant fraction of the volume. In a fluid-free environment, heat cannot conduct through voids; only radiation can transfer energy across them. We model the effective thermal conductivity of a rubble pile and show that it is proportional the square root of the pressure, $P$, for $P\leq \epsy^3\mu$ where $\epsy$ is the material's yield strain and $\mu$ its shear modulus. Our model provides an excellent fit to the depth dependence of the thermal conductivity in the top $140\,\mathrm{cm}$ of the lunar regolith. It also offers an explanation for the low thermal inertias of rocky asteroids and icy satellites. Lastly, we discuss how rubble piles slow down the cooling of small bodies such as asteroids.

Electromagnetic (EM) follow-up observations of gravitational wave (GW) events will help shed light on the nature of the sources, and more can be learned if the EM follow-ups can start as soon as the GW event becomes observable. In this paper, we propose a computationally efficient time-domain algorithm capable of detecting gravitational waves (GWs) from coalescing binaries of compact objects with nearly zero time delay. In case when the signal is strong enough, our algorithm also has the flexibility to trigger EM observation {\it before} the merger. The key to the efficiency of our algorithm arises from the use of chains of so-called Infinite Impulse Response (IIR) filters, which filter time-series data recursively. Computational cost is further reduced by a template interpolation technique that requires filtering to be done only for a much coarser template bank than otherwise required to sufficiently recover optimal signal-to-noise ratio. Towards future detectors with sensitivity extending to lower frequencies, our algorithm's computational cost is shown to increase rather insignificantly compared to the conventional time-domain correlation method. Moreover, at latencies of less than hundreds to thousands of seconds, this method is expected to be computationally more efficient than the straightforward frequency-domain method.

Efeitos da associação da ovariectomia com uma dieta hiperlipídica sobre alterações no metabolismo lipídico, remodelamento e redistribuição do tecido adiposo e sobre os marcadores inflamatórios em camundongas C57BL/6

A menopausa está associada a algumas alterações metabólicas como a obesidade, dislipidemia e inflamação, entre outras anomalias presentes na síndrome metabólica humana. Uma dieta hiperlipídica ou high-fat (HF) associada à menopausa piora tais alterações, aumentando ainda mais o risco de doença cardiovascular. A hipótese de que uma dieta HF agrava as complicações relacionadas à ovariectomia foi testada. Foram avaliadas fêmeas C57BL/6 ovariectomizadas (OVX) ou com operação SHAM e alimentados com ração padrão ou Standard Chow (SC, 10% de gordura) ou uma dieta HF (60% de gordura) por 18 semanas. A eficiência alimentar (EA), massa corporal (MC), distribuição regional das massas de gordura e a morfometria dos adipócitos foram estudados. As análises de sangue (colesterol total, CT, triglicerídeos, TG, citocinas e adipocinas) foram realizadas. Camundongas OVX-HF apresentaram maior EA e maior MC do que os demais grupos (P<0,05). A gordura visceral (ovariana e retroperitoneal) e a gordura subcutânea (gordura inguinal) tiveram o mesmo padrão de distribuição entre os grupos SHAM-SC, SHAM-HF e OVX-SC, mas o grupo OVX-HF apresentou um padrão diferente de acúmulo de gordura - muito maior do que no rupo SHAM-SC. A associação da ovariectomia com a dieta HF aumentou significativamente o diâmetro dos adipócitos dos animais OVX-HF em comparação aos SHAM-HF (P<0,0001) e também agravou a elevação dos níveis de CT, TG e de leptina nas camundongas OVX-HF, em relação aos OVX-SC (P<0,0001). Os níveis de adiponectina foram maiores nas camundongas OVX-SC comparados com as das camundongas SHAM-SC e OVX-HF (P<0,001). A associação da ovariectomia com a dieta HF agravou o aumento dos níveis séricos de leptina em camundongas OVX-HF, em relação aos OVX-SC (P<0,005). TNF-alfa não foi diferente entre os grupos, mas a IL-6 foi significativamente maior nas camundongas OVX-HF comparados a ambos os grupos SHAM-HF e OVX-SC (P<0,0001). Concluindo, a ingestão de uma dieta hiperlipídica por camundongas ovariectomizadas, leva ao aumento do acúmulo e redistribuição inadequada de gordura, à piora dos níveis de citocinas e adipocinas, assim como à desordem metabólica, o que aumenta os fatores de risco para doenças cardiovasculares.

Tenacificação em Nanocompósitos de Poliamida 6 e Argila

Nanocompósitos de poliamida 6 (PA6) e montmorilonita modificada com sal de amônio quaternário têm sido estudados, visando melhorar as propriedades térmicas e mecânicas. De fato os efeitos da nano-escala e da interação carga-matriz resultam em maior módulo de elasticidade e resistência à tração, porém a deformação é reduzida. Assim, nesse trabalho, optou-se por adicionar elastômeros, terpolímero de etileno-propileno-dieno (EPDM) e terpolímero de etileno-propileno-dieno modificado com anidrido maleico (EPDM-MA), ao sistema PA 6/argila organofílica para recuperar os valores de deformação. Foi utilizada montmorilonita modificada com cloreto de dimetildioctadecil amônio. A intercalação por fusão foi realizada em câmara interna de mistura. Além das propriedades mecânicas, térmicas e reológicas, foram investigadas as modificações na cristalinidade da fase PA-6 em função da adição da argila modificada, EPDM e EPDM-MA, detectando-se as variações no grau de cristalinidade e nas temperaturas de fusão e cristalização. Os difratogramas de raios-x revelaram ocorrência de intercalação/esfoliação e também modificação da forma cristalina da PA 6, indicando a formação do cristal gama