Abundance and biomass of planktonic diatom Proboscia alata and associated species, chlorophyll a, organic carbon and nitrogen concentrations in waters over the Bering Sea middle shelf in August 2001

During most of the vegetation season from late May to early September large-sized diatom alga Proboscia alata forms local patches with high abundances and biomasses in different oceanographic domains of the eastern Bering Sea shelf. For 0-25 m layer average abundance and biomass of species in these patches are 700000 cells/l and 5 g/m**3 (wet weight), while corresponding estimates for the layer of maximal species concentrations are 40000000 cells/l and 38 g/m**3 (wet weight) or 1.6 g C/m**3. These levels of abundance and biomass are typical for the spring diatom bloom in the region. Outbursts of P. alata mass development are important for the carbon cycle in the pelagic zone of the shelf area in the summer season. The paradox of P. alata summertime blooms over the middle shelf lies in their occurrences against the background of the sharp seasonal pycnocline and deficiency in nutrients in the upper mixed layer. Duration of the outbursts in P. alata development is about two weeks and size of patches with high abundances can be as large as 200 km across. Degradation of the P. alata summertime outbursts may occur during 4-5 days. Rapid sinking of cells through the seasonal pycnocline results in intense transport of organic matter to bottom sediments. One of possible factors responsible for rapid degradation of the blooms is affect on the population by ectoparasitic flagellates. At terminal stages of the P. alata blooms percentage of infected cells can reach 70-99%.

Biomarker and x-ray diffraction data from Site U1313 (MIS 16 - 9)

A reconstruction of Milankovitch to millennial-scale variability of sea-surface temperature (SST) and sea-surface productivity in the Pleistocene mid-latitude North Atlantic Ocean (MIS 16-9) and its relationship to ice sheet instability was carried out on sediments from IODP Site U1313. This reconstruction is based on alkenone and n-alkane concentrations, Uk37' index, total organic carbon (TOC) and carbonate contents, X-Ray diffraction (XRD) data, magnetic susceptibility, and accumulation rates. Increased input of ice-rafted debris (IRD) occurred during MIS 16, 12, and 10, characterized by high concentrations of dolomite, quartz, and feldspars and elevated accumulation rates of terrigenous matter. Minimum input values of terrigenous matter, on the other hand, were determined for MIS 13 and 11. Peak values of dolomite, coinciding with quartz, plagioclase, and kalifeldspar peaks and maxima in long-chain n-alkanes indicative for land plants, are interpreted as Heinrich-like Events related to sudden instability of the Laurentide Ice Sheet during early and late (deglacial) phases of the glacials. The coincidence of increased TOC values with elevated absolute concentrations of alkenones suggest increased glacial productivity, probably due to a more southern position of the Polar Front. Alkenone-based SST reached absolute maxima of about 19°C during MIS 11.3 and absolute minima of <10°C during MIS 12 and 10. Within MIS 11, prominent cooling events (MIS 11.22 and 11.24) occurred. The absolute SST minima recorded directly before and after the glacial maxima MIS 10.2 and 12.2, are related to Heinrich-like Event meltwater pulses, as supported by the coincidence of SST minima and maxima in C37:4 alkenones and dolomite. These sudden meltwater pulses - especially during Terminations IV and V - probably caused a collapse of phytoplankton productivity as indicated by the distinct drop in alkenone concentrations. Ice-sheet disintegration and subsequent surges and outbursts of icebergs and meltwater discharge may have been triggered by increased insolation in the Northern High Latitudes.

A silviculture-oriented spatio-temporal model for germination in Pinus pinea L. in the Spanish Northern Plateau based on a direct seeding experiment

Natural regeneration in Pinus pinea stands commonly fails throughout the Spanish Northern Plateau under current intensive regeneration treatments. As a result, extensive direct seeding is commonly conducted to guarantee regeneration occurrence. In a period of rationalization of the resources devoted to forest management, this kind of techniques may become unaffordable. Given that the climatic and stand factors driving germination remain unknown, tools are required to understand the process and temper the use of direct seeding. In this study, the spatio-temporal pattern of germination of P. pinea was modelled with those purposes. The resulting findings will allow us to (1) determine the main ecological variables involved in germination in the species and (2) infer adequate silvicultural alternatives. The modelling approach focuses on covariates which are readily available to forest managers. A two-step nonlinear mixed model was fitted to predict germination occurrence and abundance in P. pinea under varying climatic, environmental and stand conditions, based on a germination data set covering a 5-year period. The results obtained reveal that the process is primarily driven by climate variables. Favourable conditions for germination commonly occur in fall although the optimum window is often narrow and may not occur at all in some years. At spatial level, it would appear that germination is facilitated by high stand densities, suggesting that current felling intensity should be reduced. In accordance with other studies on P. pinea dispersal, it seems that denser stands during the regeneration period will reduce the present dependence on direct seeding.

Metodología de rehabilitación energética de barrios y regeneración urbana: aplicación al barrio Almenara

El origen de la investigación se basa en la necesid ad de intervención a nivel ambiental, económico y social, en el barrio Almenara de Tetuán , Madrid. El objetivo principal de la investigación es la búsqueda de una metodología de rehabilitación energética de barrios y regeneración urbana. Los objetivos secundarios so n la aplicación de la metodología al barrio reduciendo las demandas energéticas de modo directo, mediante la mejora de los parámetros característicos de la envolvente, y de m odo indirecto, mediante la aplicación de materiales fríos en cubierta y fachada, la intro ducción de envolventes vegetales, que aumenten la evapotranspiración y reduzcan la temper atura ambiental y la modificación de la morfología de la cubierta, incorporando zonas de estancia. Todo ello, en busca de un espacio urbano global. La metodología de trabajo comenzó con la caracterización histórica y normativa del área por medio de la cons ulta de publicaciones del Ministerio y Gerencia de Urbanismo. Y la caracterización edifica toria del barrio por medio de los Archivos de Documentación histórica. Desde el punto de vista medioambiental, se ha realizado un análisis climático, a partir de la dir ección y velocidad de los vientos y la radiación solar recibida por las superficies estruc turantes de pavimentación y cubiertas, así como las fachadas en los solsticios y equinocci os. Todo ello, analizando la localización de las zonas verdes actuales y futuras y su influen cia. Se ha analizado la movilidad del transporte público, la influencia de los ciclistas y accesibilidad de personas con movilidad reducida. Se han obtenido las lesiones como parámet ros en términos de condicionamiento térmico, a nivel urbano y edificat orio y se ha realizado un trabajo a nivel termográfico de la edificación. El análisis s ocial y poblacional se ha obtenido mediante una encuesta de elaboración propia sobre e l estado actual de la edificación, las condiciones de confort de los inquilinos, y la obte nción de indicadores de Vulnerabilidad Urbana a través de la aplicación de cartografía din ámica online denominada “Atlas de Vulnerabilidad Urbana de España”. Finalmente, se ha aplicado todo lo anterior al barrio Almenara a nivel urbano y edificatorio, sobre una m anzana residencial tipo, y sobre una vivienda característica, desde el punto de vista me dioambiental, económico y social.

Estudo da influência do relacionamento entre a égua e o potro no comportamento social e no temperamento de potros da raça Mangalarga Marchador

O trabalho teve como objetivo compreender o relacionamento entre a égua e o potro e a influência deste sobre o comportamento social e temperamento do potro, a partir do décimo primeiro dia de vida até após o processo de desmama do potro. Oito díades de éguas e potros da raça Mangalarga Marchador provenientes de um criatório situado na cidade de Amparo/SP foram avaliadas durante três etapas distintas. A primeira foi realizada para caracterizar o comportamento social do grupo de equinos e o relacionamento entre égua e potro durante os três períodos de desenvolvimento do potro (dependência, socialização e independência). Nessa etapa foram registradas: as interações agonísticas das éguas; episódios de mamada dos potros (tentativas e mamadas) e para o par égua e potro foram anotados os comportamentos afiliativos e a relação espacial. Ao final dessa etapa os potros foram classificados em dependentes e independentes e as éguas foram divididas de acordo com sua hierarquia. A segunda etapa constitui-se da avaliação das atividades e relação espacial dos potros durante o processo de desmama, para a caracterização do estresse dos potros. Na terceira etapa a relação social dos potros foi observada na ausência de suas mães, através do registro das interações e da relação espacial dos potros. Durante as três etapas foram aplicados quatro testes de avaliação dos aspectos do temperamento dos animais: teste de reatividade durante o manejo de escovação para a avaliação da reatividade ao manejo; teste de arena para avaliar a emotividade ao isolamento; teste de reatividade perante humano desconhecido e ativo para avaliar a reatividade ao humano; e teste da presença de estímulo sonoro desconhecido para avaliação da emotividade ao estímulo desconhecido. A hierarquia e a experiência da mãe interferiam no cuidado materno de aleitamento (P<0,05), entretanto, não influenciaram o cuidado de proteção (P>0,05). A frequência de permanência dos potros com sua mãe na distância de até 1 metro diminuiu ao longo dos períodos (P<0,05). As éguas não modificaram a frequência dos comportamentos afiliativos com seus potros ao longo dos períodos (P>0,05). As maiores frequências de comportamentos afiliativos dos potros com suas mães foram durante os períodos iniciais do desenvolvimento do potro (dependência e socialização, P<0,05). Potros dependentes apresentaram maior frequência e menor duração das mamadas quando comparado à frequência e duração dos potros independentes (P<0,05). A reatividade ao manejo e a emotividade ao isolamento dos potros foram maiores nos períodos da dependência, da socialização e durante a desmama (P<0,05). A reatividade ao humano e emotividade ao desconhecido apresentaram a tendência de diminuir ao longo dos períodos observados (P<0,05). Os potros dependentes apresentaram maior emotividade ao desconhecido e ao isolamento (P<0,05), além de maior estresse durante a desmama, quando comparado aos potros independentes. Todos os potros normalizaram suas atividades no decorrer do processo da desmama. Na ausência das mães os potros independentes foram os que iniciaram a maioria das interações entre os animais (P<0,05). O relacionamento entre a égua e o potro foi modificado devido às características maternas de hierarquia e experiência, além do nível de independência do potro e do seu temperamento.

Trauma Treatment in Forensic Settings: Clinicians' Perspectives, Barriers to Effective Treatment, and Suggestions for Clinical Practice

Between 30% and 90% of the prison population is estimated to have survived traumatic experiences such as sexual, emotional, and physical abuse prior to incarceration (Anonymous, 1999; Fondacaro, Holt, & Powell, 1999; Messina & Grella, 2006; Pollard & Baker, 2000; Veysey, De Cou, & Prescott, 1998). Similarly, information from the Bureau of Justice Statistics (as reported in Warren, 2001) estimated that more than half of the women in state prisons have experienced past physical and sexual abuse. Thus, given the astonishing number of inmates who appear to be victims of some kind of trauma, it seems likely that those who work with these inmates (e.g., prison staff, guards, and treatment providers) will in some way encounter challenges related to the inmates' trauma history. These difficulties may appear in any number of forms including inmates' behavioral outbursts, increased emotionality, sensitivity to triggering situations, and chronic physical or mental health needs (Veysey, et al., 1998). It is also likely that these individuals with trauma histories would benefit greatly from treatment while incarcerated. This treatment could be utilized to minimize symptoms of posttraumatic stress, decrease behavioral problems, and help the inmate function more effectively in society when released from incarceration (Kokorowski & Freng, 2001; Tucker, Cosio, Meshreki, 2003). Few studies have explored the types of trauma treatment that are effective with inmate populations or made specific suggestions for clinicians working in forensic settings (Kokorowski & Freng, 2001). Essentially, there appears to be a large gap in terms of the need for trauma treatment for inmates and the lack of literature addressing what to do about it. However, clinicians across the country seem to be quietly attempting to fulfill this need for trauma treatment with incarcerated populations. They are providing this greatly needed treatment every day. in the face of enormous challenges and often without recognition or the opportunity to share their valuable work with the larger community.

Consequences of the Past: China's Rise to Superpower Status and its Impact on the United States

This paper investigates the impact of how the Chinese government will react to the West if China regains its superpower status. Using traditional research methods, this paper traced the cultural misunderstandings that initiated the confrontation with the West and the resulting humiliation China suffered for nearly 175 years by the Western powers. The findings of this paper show that China bitterly resents the treatment suffered during the Colonial period. Although certain factions in China wish to punish the West, this paper argues that the interconnected nature of the world's economy will force China to temper its feelings and build bridges with the West as it attains superpower status.

On the nature of candidate luminous blue variables in M 33

Context. Luminous blue variables (LBVs) are a class of highly unstable stars that have been proposed to play a critical role in massive stellar evolution as well as being the progenitors of some of the most luminous supernovae known. However the physical processes underlying their characteristic instabilities are currently unknown. Aims. In order to provide observational constraints on this behaviour we have initiated a pilot study of the population of (candidate) LBVs in the Local Group galaxy M 33. Methods. To accomplish this we have obtained new spectra of 18 examples within M 33. These provide a baseline of ≥ 4 yr with respect to previous observations, which is well suited to identifying LBV outbursts. We also employed existing multi-epoch optical and mid-IR surveys of M 33 to further constrain the variability of the sample and search for the presence of dusty ejecta. Results. Combining the datasets reveals that spectroscopic and photometric variability appears common, although in the majority of cases further observations will be needed to distinguish between an origin for this behavour in short lived stochastic wind structure and low level photospheric pulsations or coherent long term LBV excursions. Of the known LBVs we report a hitherto unidentified excursion of M 33 Var C between 2001-5, while the transition of the WNLh star B517 to a cooler B supergiant phase between 1993−2010 implies an LBV classification. Proof-of-concept quantitative model atmosphere analysis is provided for Romano’s star; the resultant stellar parameters being consistent with the finding that the LBV excursions of this star are accompanied by changes in bolometric luminosity. The combination of temperature and luminosity of two stars, the BHG [HS80] 110A and the cool hypergiant B324, appear to be in violation of the empirical Humphreys-Davidson limit. Mid-IR observations demonstrate that a number of candidates appear associated with hot circumstellar dust, although no objects as extreme as η Car are identified. The combined dataset suggests that the criteria employed to identify candidate LBVs results in a heterogeneous sample, also containing stars demonstrating the B[e] phenomenon. Of these, a subset of optically faint, low luminosity stars associated with hot dust are of particular interest since they appear similar to the likely progenitor of SN 2008S and the 2008 NGC 300 transient (albeit suffering less intrinsic extinction). Conclusions. The results of such a multiwavelength observational approach, employing multiplexing spectrographs and supplemented with quantitative model atmosphere analysis, appears to show considerable promise in both identifying and characterising the physical properties of LBVs as well as other short lived phases of massive stellar evolution.

GRO J1008−57: an (almost) predictable transient X-ray binary

A study of archival RXTE, Swift, and Suzaku pointed observations of the transient high-mass X-ray binary GRO J1008−57 is presented. A new orbital ephemeris based on pulse arrival-timing shows the times of maximum luminosities during outbursts of GRO J1008−57 to be close to periastron at orbital phase − 0.03. This makes the source one of a few for which outburst dates can be predicted with very high precision. Spectra of the source in 2005, 2007, and 2011 can be well described by a simple power law with high-energy cutoff and an additional black body at lower energies. The photon index of the power law and the black-body flux only depend on the 15–50 keV source flux. No apparent hysteresis effects are seen. These correlations allow us to predict the evolution of the pulsar’s X-ray spectral shape over all outbursts as a function of just one parameter, the source’s flux. If modified by an additional soft component, this prediction even holds during GRO J1008−57’s 2012 type II outburst.

Fast X-ray transients towards the Galactic bulge with the Rossi X-ray Timing Explorer

In X-ray binaries, rapid variability in X-ray flux of greater than an order of magnitude on time-scales of a day or less appears to be a signature of wind accretion from a supergiant companion. When the variability takes the form of rare, brief, bright outbursts with only faint emission between them, the systems are called supergiant fast X-ray transients (SFXTs). We present data from twice-weekly scans of the Galactic bulge by the Rossi X-ray Timing Explorer that allow us to compare the behaviour of known SFXTs and possible SFXT candidates with the persistently bright supergiant X-ray binary 4U 1700−377. We independently confirm the orbital periods reported by other groups for SFXTs SAX J1818.6−1703 and IGR J17544−2619. The new data do not independently reproduce the orbital period reported for XTE J1739−302, but slightly improve the significance of the original result when the data are combined. The bulge source XTE J1743−363 shows a combination of fast variability and a long-term decline in activity, the latter behaviour not being characteristic of supergiant X-ray binaries. A far-red spectrum of the companion suggests that it is a symbiotic neutron star binary rather than a high-mass binary, and the reddest known of this class: the spectral type is approximately M8 III.

Astrophysical parameters of the peculiar X-ray transient IGR J11215−5952

Context. The current generation of X-ray satellites has discovered many new X-ray sources that are difficult to classify within the well-described subclasses. The hard X-ray source IGR J11215−5952 is a peculiar transient, displaying very short X-ray outbursts every 165 days. Aims. To characterise the source, we obtained high-resolution spectra of the optical counterpart, HD 306414, at different epochs, spanning a total of three months, before and around the 2007 February outburst with the combined aims of deriving its astrophysical parameters and searching for orbital modulation. Methods. We fit model atmospheres generated with the fastwind code to the spectrum, and used the interstellar lines in the spectrum to estimate its distance. We also cross-correlated each individual spectrum to the best-fit model to derive radial velocities. Results. From its spectral features, we classify HD 306414 as B0.5 Ia. From the model fit, we find Teff ≈ 24 700 K and log g ≈ 2.7, in good agreement with the morphological classification. Using the interstellar lines in its spectrum, we estimate a distance to HD 306414 d ≳ 7 kpc. Assuming this distance, we derive R∗ ≈ 40 R⊙ and Mspect ≈ 30 M⊙ (consistent, within errors, with Mevol ≈ 38 M⊙, and in good agreement with calibrations for the spectral type). Analysis of the radial velocity curve reveals that radial velocity changes are not dominated by the orbital motion, and provide an upper limit on the semi-amplitude for the optical component Kopt ≲ 11 ± 6 km   s-1. Large variations in the depth and shape of photospheric lines suggest the presence of strong pulsations, which may be the main cause of the radial velocity changes. Very significant variations, uncorrelated with those of the photospheric lines are seen in the shape and position of the Hα emission feature around the time of the X-ray outburst, but large excursions are also observed at other times. Conclusions. HD 306414 is a normal B0.5 Ia supergiant. Its radial velocity curve is dominated by an effect that is different from binary motion, and is most likely stellar pulsations. The data available suggest that the X-ray outbursts are caused by the close passage of the neutron star in a very eccentric orbit, perhaps leading to localised mass outflow.

Astrophysical parameters and orbital solution of the peculiar X-ray transient IGR J00370+6122

Context. BD + 60° 73 is the optical counterpart of the X-ray source IGR J00370+6122, a probable accretion-powered X-ray pulsar. The X-ray light curve of this binary system shows clear periodicity at 15.7 d, which has been interpreted as repeated outbursts around the periastron of an eccentric orbit. Aims. We aim to characterise the binary system IGR J00370+6122 by deriving its orbital and physical parameters. Methods. We obtained high-resolution spectra of BD + 60° 73 at different epochs. We used the fastwind code to generate a stellar atmosphere model to fit the observed spectrum and obtain physical magnitudes. The synthetic spectrum was used as a template for cross-correlation with the observed spectra to measure radial velocities. The radial velocity curve provided an orbital solution for the system. We also analysed the RXTE/ASM and Swift/BAT light curves to confirm the stability of the periodicity. Results. BD + 60° 73 is a BN0.7 Ib low-luminosity supergiant located at a distance ~3.1 kpc, in the Cas OB4 association. We derive Teff = 24 000 K and log gc = 3.0, and chemical abundances consistent with a moderately high level of evolution. The spectroscopic and evolutionary masses are consistent at the 1-σ level with a mass M∗ ≈ 15 M⊙. The recurrence time of the X-ray flares is the orbital period of the system. The neutron star is in a high-eccentricity (e = 0.56 ± 0.07) orbit, and the X-ray emission is strongly peaked around orbital phase φ = 0.2, though the observations are consistent with some level of X-ray activity happening at all orbital phases. Conclusions. The X-ray behaviour of IGR J00370+6122 is reminiscent of “intermediate” supergiant X-ray transients, though its peak luminosity is rather low. The orbit is somewhat wider than those of classical persistent supergiant X-ray binaries, which when combined with the low luminosity of the mass donor, explains the low X-ray luminosity. IGR J00370+6122 will very likely evolve towards a persistent supergiant system, highlighting the evolutionary connection between different classes of wind-accreting X-ray sources.

The many lives of magnetized neutron stars

The magnetic field strength at birth is arguably one of the most important properties to determine the evolutionary path of a neutron star. Objects with very high fields, collectively known as magnetars, are characterized by high X-ray quiescent luminosities, occurrence of outbursts, and, for some of them, sporadic giant flares. While the magnetic field strength is believed to drive their collective behaviour, however, the diversity of their properties, and, especially, the observation of magnetar-like bursts from “low-field” pulsars, has been a theoretical puzzle. In this review, we discuss results of long-term simulations following the coupled evolution of the X-ray luminosity and the timing properties for a large, homogeneous sample of X-ray emitting isolated neutron stars, accounting for a range of initial magnetic field strengths, envelope compositions, and neutron star masses. In addition, by following the evolution of magnetic stresses within the neutron star crust, we can also relate the observed magnetar phenomenology to the physical properties of neutron stars, and in particular to their age and magnetic field strength and topology. The dichotomy of “high-B” field pulsars versus magnetars is naturally explained, and occasional outbursts from old, low B-field neutron stars are predicted. We conclude by speculating on the fate of old magnetars, and by presenting observational diagnostics of the neutron star crustal field topology.

Quiescent thermal emission from neutron stars in low-mass X-ray binaries

Context. We monitored the quiescent thermal emission from neutron stars in low-mass X-ray binaries after active periods of intense activity in X-rays (outbursts). Aims. The theoretical modeling of the thermal relaxation of the neutron star crust may be used to establish constraints on the crust composition and transport properties, depending on the astrophysical scenarios assumed. Methods. We numerically simulated the thermal evolution of the neutron star crust and compared them with inferred surface temperatures for five sources: MXB 1659−29, KS 1731−260, XTE J1701−462, EXO 0748−676  and IGR J17480−2446. Results. We find that the evolution of MXB 1659−29, KS 1731−260 and EXO 0748−676 can be well described within a deep crustal cooling scenario. Conversely, we find that the other two sources can only be explained with models beyond crustal cooling. For the peculiar emission of XTE J1701−462 we propose alternative scenarios such as residual accretion during quiescence, additional heat sources in the outer crust, and/or thermal isolation of the inner crust due to a buried magnetic field. We also explain the very recent reported temperature of IGR J17480−2446 with an additional heat deposition in the outer crust from shallow sources.

La nécessité d'une multiplicité de concepts de gène en biologie

Le concept de gène est central en biologie. Certains ont avancé (Ruse (1971, 1976)) que la génétique classique pouvait être réduite à la génétique moléculaire. Dans le même ordre d'idée, Richard Dawkins, dans The Extended Phenotype, offre une double définition de son concept de gène qui présuppose qu'il soit possible d'opérer cette réduction. Nous comptons montrer que la génétique moléculaire et la génétique des populations ont chacune leurs problématiques propres en reconstituant l'histoire de la génétique depuis Darwin. Ensuite, nous expliciterons la position de Dawkins et soulignerons les contradictions auxquelles il parvient en raison de cette réduction infondée. À la suite de quoi, nous nous attarderons aux nouvelles découvertes moléculaires qui montrent qu'il n'est pas possible d'opérer la réduction d'un des concepts à l'autre. Nous terminerons en soulignant que la thèse génocentriste de Dawkins n'est pas mise en péril par l'abandon de la réduction, mais qu'il est nécessaire de tempérer ces prétentions. La conclusion globale de ce mémoire est qu'il est possible d'admettre le concept de Dawkins, mais pas la manière dont il l'utilise. Le concept est bon, il n'est tout simplement pas dans le bon cadre théorique.