Field measurements of the atmosphere, ocean, sea ice and sub-ice platelet layer at Atka Bay in 2013

Ice shelves strongly interact with coastal Antarctic sea ice and the associated ecosystem by creating conditions favourable to the formation of a sub-ice platelet layer. The close investigation of this phenomenon and its seasonal evolution remain a challenge due to logistical constraints and a lack of suitable methodology. In this study, we characterize the seasonal cycle of Antarctic fast ice adjacent to the Ekström Ice Shelf in the eastern Weddell Sea. We used a thermistor chain with the additional ability to record the temperature response induced by cyclic heating of resistors embedded in the chain. Vertical sea-ice temperature and heating profiles obtained daily between November 2012 and February 2014 were analyzed to determine sea-ice and snow evolution, and to calculate the basal energy budget. The residual heat flux translated into an ice-volume fraction in the platelet layer of 0.18 ± 0.09, which we reproduced by a independent model simulation and agrees with earlier results. Manual drillings revealed an average annual platelet-layer thickness increase of at least 4m, and an annual maximum thickness of 10m beneath second-year sea ice. The oceanic contribution dominated the total sea-ice production during the study, effectively accounting for up to 70% of second-year sea-ice growth. In summer, an oceanic heat flux of 21 W/m**2 led to a partial thinning of the platelet layer. Our results further show that the active heating method, in contrast to the acoustic sounding approach, is well suited to derive the fast-ice mass balance in regions influenced by ocean/ice-shelf interaction, as it allows sub-diurnal monitoring of the platelet-layer thickness.

Self-similar motion of laser half-space plasmas. I. Deflagration regime

The one-dimensional self-similar motion of an initially cold, half-space plasma of electron density 0,produced by the (anomalous) absorption of a laser pulse of irradiation = (j>0f/T(0< (< T) at the critical density nc(«c/«0=eoKe)213, where k, m, are Boltzmann's constant and the ion mass, and Ke X (electron temperature)5'2 = heat conductivity. If a >e- 4 ' 3 , a deflagration wave separates an isentropic compression with a shock bounding the undisturbed plasma, and an isentropic expansion flow to the vacuum. The structures of these three regions are completely determined; in particular, the Chapman-Jouguet condition is proved and the density behind the deflagration is found. The deflagration-compression thickness ratio is large (small) for a^e- 5 ' 3(a>e- 5 ' 3 ) . The compression to expansion ratio for both energy and thickness is 0(e"2). For Z,- large, a deflagration exists even if a~e~413. Condition a>e~4'3 may be applied to pulses that are not linear.

Centuria primera del real y militar instituto de la inclita religion de Nuestra Señora de la Merced Redempcion de cautivos christianos : parte primera ...

Índices

Parte del Atlas Mayor o Geographia Blauiana, que contiene las cartas y descripciones de España [Texto impreso]

Hay variantes de esta ed. en: port. tip. por la presencia de banderilla "de las" en el tít. y en el front. por ausencia de datos; prelim. y algunas p. del cuerpo de obra por composición diferente; el map. de la Península puede aparecer rodeado de otros grab.; hay ejemp. coloreados a mano y otros no

Estudo do comportamento eletroquímico da liga UNS N07090 em diferentes concentrações de ácido sulfúrico.

Ligas de níquel têm atualmente uma vasta gama de aplicações, sendo a agressividade do meio e as elevadas temperaturas que estas ligas suportam, um diferencial excepcional. A liga UNS N07090, objeto deste trabalho, encontra aplicações muito diversas, entre elas turbocompressores, sistemas de exaustão e de pós-tratamento de motores a diesel. Nestas aplicações a liga está exposta a gases, que ao condensarem formam ácido sulfúrico (H2SO4). Torna-se, assim, importante, o conhecimento da resistência à corrosão da liga nesse meio. O presente trabalho tem como objetivo caracterizar o comportamento eletroquímico da liga através de curvas de polarização potenciodinâmica em diferentes concentrações de ácido sulfúrico. Observou-se que quanto maior a concentração de ácido, maior é a corrosão da liga. Este fato pode ser discutido pela adsorção do íon sulfato (SO42-), que prejudica tanto a formação quanto a cinética de crescimento da película passiva do níquel. Em contrapartida, a presença de Cr na liga UNS N07090 apresentou um benefício sobre a resistência à corrosão desta muito acima do esperado, influenciando de forma direta as curvas de polarização da liga e mantendo-a em condição de elevada resistência à corrosão em detrimento do pior desempenho observado em outros elementos pertecentes à liga, como Co, Al e Ti. Tempos de imersão de 24h em ácido sulfúrico elevam discretamente os parâmetros de corrosão da liga, mantendo-os, no entanto em patamares bastante baixos, permitindo finalmente concluir que a liga UNS N07090, quando exposta a concentrações que variam de 1M a 4M H2SO4, a 25°C, apresenta boa resistência à corrosão e que esta não se altera com o tempo de exposição. A análise dos resultados mostrou que o processo corrosivo é controlado por reações catódicas de sulfato e hidrogênio, as quais podem ter diferentes contribuições dependendo da concentração do ácido e do tempo de imersão da liga UNS N07090 no meio corrosivo.

The circumstellar environment and evolutionary status of the supergiant B[e] star Wd1-9

Context. Historically, supergiant (sg)B[e] stars have been difficult to include in theoretical schemes for the evolution of massive OB stars. Aims. The location of Wd1-9 within the coeval starburst cluster Westerlund 1 means that it may be placed into a proper evolutionary context and we therefore aim to utilise a comprehensive multiwavelength dataset to determine its physical properties and consequently its relation to other sgB[e] stars and the global population of massive evolved stars within Wd1. Methods. Multi-epoch R- and I-band VLT/UVES and VLT/FORS2 spectra are used to constrain the properties of the circumstellar gas, while an ISO-SWS spectrum covering 2.45−45μm is used to investigate the distribution, geometry and composition of the dust via a semi-analytic irradiated disk model. Radio emission enables a long term mass-loss history to be determined, while X-ray observations reveal the physical nature of high energy processes within the system. Results. Wd1-9 exhibits the rich optical emission line spectrum that is characteristic of sgB[e] stars. Likewise its mid-IR spectrum resembles those of the LMC sgB[e] stars R66 and 126, revealing the presence of equatorially concentrated silicate dust, with a mass of ~10−4M⊙. Extreme historical and ongoing mass loss (≳ 10−4M⊙yr−1) is inferred from the radio observations. The X-ray properties of Wd1-9 imply the presence of high temperature plasma within the system and are directly comparable to a number of confirmed short-period colliding wind binaries within Wd1. Conclusions. The most complete explanation for the observational properties of Wd1-9 is that it is a massive interacting binary currently undergoing, or recently exited from, rapid Roche-lobe overflow, supporting the hypothesis that binarity mediates the formation of (a subset of) sgB[e] stars. The mass loss rate of Wd1-9 is consistent with such an assertion, while viable progenitor and descendent systems are present within Wd1 and comparable sgB[e] binaries have been identified in the Galaxy. Moreover, the rarity of sgB[e] stars - only two examples are identified from a census of ~ 68 young massive Galactic clusters and associations containing ~ 600 post-Main Sequence stars - is explicable given the rapidity (~ 104yr) expected for this phase of massive binary evolution.

MY Camelopardalis, a very massive merger progenitor

Context. The early-type binary MY Cam belongs to the young open cluster Alicante 1, embedded in Cam OB3. Aims. MY Cam consists of two early-O type main-sequence stars and shows a photometric modulation suggesting an orbital period slightly above one day. We intend to confirm this orbital period and derive orbital and stellar parameters. Methods. Timing analysis of a very exhaustive (4607 points) light curve indicates a period of 1.1754514 ± 0.0000015 d. High-resolution spectra and the cross-correlation technique implemented in the todcor program were used to derive radial velocities and obtain the corresponding radial velocity curves for MY Cam. Modelling with the stellar atmosphere code fastwind was used to obtain stellar parameters and create templates for cross-correlation. Stellar and orbital parameters were derived using the Wilson-Devinney code, such that a complete solution to the binary system could be described. Results. The determined masses of the primary and secondary stars in MY Cam are 37.7 ± 1.6 and 31.6 ± 1.4M⊙, respectively. The corresponding temperatures, derived from the model atmosphere fit, are 42 000 and 39 000 K, with the more massive component being hotter. Both stars are overfilling their Roche lobes, sharing a common envelope. Conclusions. MY Cam contains the most massive dwarf O-type stars found so far in an eclipsing binary. Both components are still on the main sequence, and probably not far from the zero-age main sequence. The system is a likely merger progenitor, owing to its very short period.

Barcelona, Spain : Street Centerlines, 2005

Barcelona, Spain street centerline vectors with road type attributes extracted from DigitalGlobe QuickBird CitySphere high-resolution (60cm) satellite imagery ortho mosaics.

Berlin, Germany : Street Centerlines, 2006

Berlin, Germany street centerline vectors with road type attributes extracted from DigitalGlobe QuickBird CitySphere high-resolution (60cm) satellite imagery ortho mosaics.

Madrid, Spain : Street Centerlines, 2005

Madrid, Spain street centerline vectors with road type attributes extracted from DigitalGlobe QuickBird CitySphere high-resolution (60cm) satellite imagery ortho mosaics.

Paris, France : Street Centerlines, 2006

Paris, France street centerline vectors with road type attributes extracted from DigitalGlobe QuickBird CitySphere high-resolution (60cm) satellite imagery ortho mosaics.

Nairobi, Kenya : Street Centerlines, 2006

Nairobi, Kenya street centerline vectors with road type attributes extracted from DigitalGlobe QuickBird CitySphere high-resolution (60cm) satellite imagery ortho mosaics.

London and vicinity, England : Street Centerlines, 2006

London, England street centerline vectors with road type attributes extracted from DigitalGlobe QuickBird CitySphere high-resolution (60cm) satellite imagery ortho mosaics.