Padrões geoacústicos de fundo e sub-fundo na Baía de Sepetiba: implicações no conhecimento da geologia do holoceno

A Baía de Sepetiba, localizada entre a Baía de Guanabara e a Baía de Ilha Grande, Estado do Rio de Janeiro, está inserida em um cenário estratégico para o desenvolvimento econômico do Estado. Isto ocorre devido ao aumento da concentração populacional, que está diretamente relacionado com o turismo, com a presença de portos e de áreas industriais. Sendo assim, se faz necessário estudar sua estrutura geológica e dinâmica sedimentar para entender sua evolução ao longo do tempo e para uma utilização mais racional desta área. Utilizando-se da sísmica rasa de alta resolução e da sonografia de varredura lateral juntamente com dados pretéritos de amostragem superficial de sedimentos, o presente trabalho tem como objetivo principal analisar sua geologia holocênica. A investigação, em subsuperfície, da geologia estrutural e sedimentar dessa baía, através da interpretação de 09 perfis sísmicos, baseada na determinação de diferentes tipos de ecotexturas, revelou a presença de diferentes pacotes sedimentares depositados ao longo do Holoceno. Ao todo, foram encontrados 15 tipos de ecotexturas perfazendo 14 camadas sedimentares, que estão relacionados em 4 Grupos de acordo com sua distribuição. Já a investigação em superfície através dos registros sonográficos, baseada nos diferentes graus de reflexão acústica (backscattering) e parametrizada pelos dados de amostragem direta pretérita, identificou 6 padrões sonográficos distintos. Com isso foi confeccionado um novo mapa de distribuição textural dos sedimentos superficiais da Baía de Sepetiba. Com a correlação dos dados de sísmica rasa com os dados sonográficos, foi possível ainda sugerir a provável existência de neotectonismo na área de estudo.

Geologia bizirik. GeoBizirik.org

Geologia Lurra aztertzen duen zientzia da: lurraren osaera, egitura eta jatorria, eta bai arroketan aztarnak utzi dituzten iraganeko edo gaur egungo gertaerak ere. Baina, zergatik du gizarteak geologoen beharra? Hona hemen zenbait arrazoi: - Geologoek lurrazalari eta lurpeari buruzko informazioa bildu, eta interpretatu egiten dute. Informazio horrek guztiak ahalbidetzen du planetaren iraganeko historia, Lurrean aurreikus daitezkeen aldaketak eta gure planetak Eguzki-sistemarekin duen harremana finkatzea. - Gizarteak beharrezkoak ditu baliabide naturalak (metalikoak, ez-metalikoak, ura eta erregai fosilak). Geologoen parte-hartzea erabakigarria da hobi berriak aurkitzeko eta ingurumena zaintzen duten baliabide naturalen ustiapen eta kudeaketarako irizpideak ezartzeko. - Kartografia geologikoen bidez arrisku-eremuak identifikatu eta lurzoruaren erabilerak mugatzen dira. Geologoak beharrezkoak dira, beraz, lurraldearen planifikaziorako eta garapen iraunkorrerako estrategiak garatzeko. - Geologiaren ezagutzak eta informazio geologikoaren erabilera egokiak laguntzen dute bizitzak salbatzen eta lurrikarak, tsunamiak, erupzio bolkanikoak, uholdeak eta lurjausiak bezalako katastrofe naturalek eragindako diru-galerak murrizten. Halaber laguntzen dute eraikuntza-proiektuak, herri-lanak eta abar garatzen ere. Proposatutako jardueren bitartez, Zientzia Geologikoen adar desberdinen oinarrizko zenbait alderdi ezagutzera eman nahi ditugu. Horretarako, lau saio antolatu ditugu Paleontologia, Mineralogia, Petrologia eta Tektonika arloetan murgiltzeko.

Novel Evidence hat Attributing Affectively Salient Signal to Random Noise Is Associated with Psychosis

We wished to replicate evidence that an experimental paradigm of speech illusions is associated with psychotic experiences. Fifty-four patients with a first episode of psychosis (FEP) and 150 healthy subjects were examined in an experimental paradigm assessing the presence of speech illusion in neutral white noise. Socio-demographic, cognitive function and family history data were collected. The Positive and Negative Syndrome Scale (PANSS) was administered in the patient group and the Structured Interview for Schizotypy-Revised (SIS-R), and the Community Assessment of Psychic Experiences (CAPE) in the control group. Patients had a much higher rate of speech illusions (33.3% versus 8.7%, ORadjusted: 5.1, 95% CI: 2.3-11.5), which was only partly explained by differences in IQ (ORadjusted: 3.4, 95% CI: 1.4-8.3). Differences were particularly marked for signals in random noise that were perceived as affectively salient (ORadjusted: 9.7, 95% CI: 1.8-53.9). Speech illusion tended to be associated with positive symptoms in patients (ORadjusted: 3.3, 95% CI: 0.9-11.6), particularly affectively salient illusions (ORadjusted: 8.3, 95% CI: 0.7-100.3). In controls, speech illusions were not associated with positive schizotypy (ORadjusted: 1.1, 95% CI: 0.3-3.4) or self-reported psychotic experiences (ORadjusted: 1.4, 95% CI: 0.4-4.6). Experimental paradigms indexing the tendency to detect affectively salient signals in noise may be used to identify liability to psychosis.

Geologia da formação ferrífera do Serrote do Breu e de Alto das Pedras, Alagoas

A formação ferrífera do Serrote do Breu e de Alto das Pedras localiza-se no município de Campo Grande, Estado de Alagoas e está sendo pesquisada quanto ao seu potencial como minério de ferro. Ela está inserida em um domo de embasamento arqueano no interior da Faixa Sergipana, o Domo de Jirau de Ponciano. A área de estudo é caracterizada por dois altos topográficos denominados Serrote do Breu e Alto das Pedras, sustentados pela formação ferrífera, e que representam flancos opostos de um sinformal inclinado, com direção N60W e forte mergulho para sul, e extensão total de aproximadamente 2 km. A formação ferrífera ocorre em diversas camadas intercaladas em gnaisses quartzo-feldspáticos e em rochas metamáficas. Os primeiros foram agrupados na unidade de gnaisses quartzo-feldspáticos e as últimas na suíte intrusiva máfica-ultramáfica. Na porção interior do sinformal estão quartzitos e paragnaisses agrupados na unidade metassedimentar e cortando essas unidades há uma unidade de pegmatitos. A formação ferrífera é constituída por quartzo, hematita, anfibólio e magnetita. O anfibólio é em geral cummingtonita, mas riebeckita também ocorre subordinadamente. Os teores médios de SiO2, e Fe2O3t são 43,1% e 50,7%, respectivamente, e, assim como os demais elementos maiores, são compatíveis com outras formações ferríferas do mundo. Com base na petrografia e geoquímica de elementos terras raras os gnaisses quartzo-feldspáticos foram divididos em gnaisses bandados e gnaisses com titanita. Ambos apresentam composição riolítica e trend calcio-alcalino. Já as rochas metamáficas e metaultramáficas apresentam composição basáltica a andesítica e trend toleítico completamente dissociado daquele dos gnaisses. Acredita-se que os gnaisses quartzo-feldspáticos e as rochas metamáficas e metaultramáficas tenham se formado em ambientes tectônicos totalmente distintos, com as últimas tendo se formado provavelmente intrusivas nos primeiros.

A transit timing analysis of seven RISE light curves of the exoplanet system HAT-P-3

We present seven light curves of the exoplanet system HAT-P-3, taken as part of a transit timing programme using the rapid imager to search for exoplanets instrument on the Liverpool Telescope. The light curves are analysed using a Markov chain Monte Carlo algorithm to update the parameters of the system. The inclination is found to be i = 86.75+0.22-0.21°, the planet-star radius ratio to be Rp/R* = 0.1098+0.0010-0.0012 and the stellar radius to be R* = 0.834+0.018-0.026Rsolar, consistent with previous results but with a significant improvement in the precision. Central transit times and uncertainties for each light curve are also determined, and a residual permutation algorithm is used as an independent check on the errors. The transit times are found to be consistent with a linear ephemeris, and a new ephemeris is calculated as Tc(0) = 2454856.70118 +/- 0.00018 HJD and P = 2.899738 +/- 0.000007 d. Model timing residuals are fitted to the measured timing residuals to place upper mass limits for a hypothetical perturbing planet as a function of the period ratio. These show that we have probed for planets with masses as low as 0.33 and 1.81 M? in the interior and exterior 2:1 resonances, respectively, assuming the planets are initially in circular orbits.

Independent Discovery of the Transiting Exoplanet HAT-P-14b

We present SuperWASP observations of HAT-P-14b, a hot Jupiter discovered by Torres et al. The planet was found independently by the SuperWASP team and named WASP-27b after follow-up observations had secured the discovery, but prior to the publication by Torres et al. Our analysis of HAT-P-14/WASP-27 is in good agreement with the values found by Torres et al. and we provide additional evidence against astronomical false positives. Due to the brightness of the host star, V-mag = 10, HAT-P-14b is an attractive candidate for further characterization observations. The planet has a high impact parameter and the primary transit is close to grazing. This could readily reveal small deviations in the orbital parameters indicating the presence of a third body in the system, which may be causing the small but significant orbital eccentricity. Our results suggest that the planet may undergo a grazing secondary eclipse. However, even a non-detection would tightly constrain the system parameters.

WASP-40b: Independent Discovery of the 0.6 M Transiting Exoplanet HAT-P-27b

From WASP photometry and SOPHIE radial velocities we report the discovery of WASP-40b (HAT-P-27b), a 0.6 M planet that transits its 12th magnitude host star every 3.04 days. The host star is of late G-type or early K-type and likely has a metallicity greater than solar ([Fe/H]=0.14±0.11). The planet's mass and radius are typical of the known hot Jupiters, thus adding another system to the apparent pileup of transiting planets with periods near 3-4 days. Our parameters match those of the recent HATnet announcement of the same planet, thus giving confidence in the techniques used. We report a possible indication of stellar activity in the host star.

The spin-orbit angles of the transiting exoplanets WASP-1b, WASP-24b, WASP-38b and HAT-P-8b from Rossiter-McLaughlin observations

We present observations of the Rossiter–McLaughlin effect for the transiting exoplanets WASP-1b, WASP-24b, WASP-38b and HAT-P-8b, and deduce the orientations of the planetary orbits with respect to the host stars’ rotation axes. The planets WASP-24b, WASP-38b and HAT-P-8b appear to move in prograde orbits and be well aligned, having sky-projected spin-orbit angles consistent with zero: λ=−4°.7 ± 4°.0, 15°+33−43 and Graphic, respectively. The host stars have Teff < 6250 K and conform with the trend of cooler stars having low obliquities. WASP-38b is a massive planet on a moderately long period, eccentric orbit so may be expected to have a misaligned orbit given the high obliquities measured in similar systems. However, we find no evidence for a large spin-orbit angle. By contrast, WASP-1b joins the growing number of misaligned systems and has an almost polar orbit, λ=Graphic. It is neither very massive, eccentric nor orbiting a hot host star, and therefore does not share the properties of many other misaligned systems.

WASP-35b, WASP-48b, and HAT-P-30b/WASP-51b: Two New Planets and an Independent Discovery of a Hat Planet

We report the detection of WASP-35b, a planet transiting a metal-poor ([Fe/H] = -0.15) star in the Southern hemisphere, WASP-48b, an inflated planet which may have spun-up its slightly evolved host star of 1.75 R sun in the Northern hemisphere, and the independent discovery of HAT-P-30b/WASP-51b, a new planet in the Northern hemisphere. Using WASP, RISE, Faulkes Telescope South, and TRAPPIST photometry, with CORALIE, SOPHIE, and NOT spectroscopy, we determine that WASP-35b has a mass of 0.72 ± 0.06 MJ and radius of 1.32 ± 0.05RJ , and orbits with a period of 3.16 days, WASP-48b has a mass of 0.98 ± 0.09 MJ , radius of 1.67 ± 0.10 RJ , and orbits in 2.14 days, while HAT-P-30b/WASP-51b, with an orbital period of 2.81 days, is found to have a mass of 0.76 ± 0.05 MJ and radius of 1.42 ± 0.03 RJ , agreeing with values of 0.71 ± 0.03 MJ and 1.34 ± 0.07 RJ reported for HAT-P-30b.