Descriptive acoustic analysis of a newly-discovered marine seep

Senior thesis written for Oceanography 445

Long-Term Lamivudine Treatment of Children with Chronic Hepatitis B: Durability of Therapeutic Responses and Safety

Lamivudine has been demonstrated safe and efficacious in the short term in a large cohort of children with chronic hepatitis B (CHB), but optimal duration of treatment has not been elucidated and limited data on the safety of long-term lamivudine administration have been reported. In addition, the durability of favourable therapeutic outcomes after lamivudine therapy in children has not been well characterized. The aim of this study was to examine the safety of lamivudine and the durability of clinical responses in a group of children who received up to 3 years of treatment for CHB. One hundred and fifty-one children from centres in nine countries who had previously received lamivudine in a large prospective trial were enrolled. During the first year, children had been randomized to either lamivudine or placebo treatment. Subsequently, in a separate extension study, those who remained hepatitis B e antigen (HBeAg) positive were given lamivudine for up to 2 years and those who were HBeAg negative were observed for additional 2 years. Results of these studies have been previously reported. In this study, these children were followed for 2 additional years. Data gathered from medical record review included weight, height, signs and symptoms of hepatitis, alanine aminotransferase (ALT) levels, serologic markers, hepatitis B virus (HBV) DNA levels and serious adverse events (SAEs). Other pharmacological treatments for CHB were allowed according to the practices of individual investigators and were documented. Subjects were divided into two groups for analysis, those who had achieved virological response (VR), defined as HBeAg negative and undetectable HBV DNA by the bDNA assay by the end of the extension study at 3 years, and those who had not. In those who had achieved VR by the end of the extension study, long-term durability of HBeAg seroconversion was 82% and >90% in those who had received lamivudine for 52 weeks and at least 2 years respectively. This compares to 75% for those who had achieved seroconversion after placebo. In those who had not achieved VR by the end of the extension study, an additional 11% did so by the end of the study; they had all received lamivudine in the previous trial, and none had received further treatment during the study. Eight children lost hepatitis B surface antigen during the study and all had received lamivudine at some point during the previous trials. Evaluation of safety data revealed no SAEs related to lamivudine. There was no effect of treatment on weight or height z scores. Clinically benign ALT flares (>10 times normal) were seen in 2% of children. Favourable outcomes from lamivudine treatment of CHB in children are maintained for at least several years after completion of treatment. Up to 3 years of lamivudine treatment is safe in children.

Acute flare induced by the calcific tendonitis of the rotator cuff: inhibition of IL-1 a potential therapeutic target?

Introduction: Calcific tendonitis of rotator cuff is observed on plainradiographs in 10% of adults, but remains asymptomatic in half thesecases. Sometimes, these calcifications induce acute flares withmassive inflammation similar to gout or CPPD crisis. Analgesics/anti-inflammatory medications are usually not sufficient to controlssymptoms in these situations. Local steroid infiltration with or withoutremoval of the calcific deposition with a needle aspiration may beuseful. A new approach could be IL-1 inhibitors. Indeed, basic calciumphosphate crystals are capable of stimulating the release of activeIL-1β in vitro. These crystals trigger IL-1β release, in an analogousmanner to MSU crystals in acute gout, suggesting that IL-1β blockademay be clinically useful.Case presentation: This report describes a 70-year old woman withacute rest pain of the right shoulder since 48 hours. On examination,we found massive limitations of active and passive movements. Thepatient evaluated, on the visual scale, her symptoms at 10/10 the nightand 5/10 the day. The radiography and showed a rounded, 8 mmcalcification in the subscapularis tendon. The ultrasound aspectrevealed a heterogeneous calcification partially non solid, surroundedby massive inflammation on Doppler. C-reactive protein anderythrocyte sedimentation rate were high (74 mg/ml, 54 mm/hour).The patient received subcutaneous injections of anakinra: 100 mgdaily for 3 days (D1-D3). We evaluated the patient in our consult at dayD1, D2, D3, D7, D16 and by phone at D70.This treatment rapidly relieved the inflammatory symptoms (within afew hours with no relapse). The mobility of the shoulder, the biologicsparameters improved and the size of the calcification as well thedegree of inflammation regressed on ultrasound after 3 days.Conclusion: This is the first report of a woman with an acute flareinduced by calcific tendonitis who received anakinra. IL-1 inhibitionmay be a therapeutic target in calcific tendonitis. To analyse thisresponse more precisely and elaborate definitive conclusions, aprospective pilot study is on-going in our ambulatory institute.

The effect of social condition and diet on the frequency of male-male agonistic displays in the field cricket, gryllus bimaculatus /

The frequency and type of agonistic displays involved in male-male encounters should be significantly influenced by the presence of females. Discrete agonistic displays vary in energy expenditure and risk, and therefore should be dependent on available resources. The influence of live females and the scent of females, on the frequency of male agonistic displays was observed in a laboratory terrarium using the field cricket Gryllus bimaculatus. The effect of energy constraints on display frequency was also determined. Half the males were fed a diet high in protein and fet; the other males were fed a lower quality diet, for a 7-11 day period. The frequency of five individual displays and mating frequency were recorded using an Event Recorder and notebook. Each group of males was presented with three experimental conditions, over three days, involving the presence or absence of live females and female scent. The presence of females elicited an increase in all displays except antennation; female scent increased the frequency of antennations, mandible flares and grapples, but to a lesser extent than did live females. The frequency of grapples significantly increased for males fed the high quality diet; however diet did not influence the other displays. The combined influence of diet and condition was significant for mandible flare only. Mating frequency was not influenced by diet. However, the frequency ofthe displays were positively correlated with mating frequency for high quality fed males. Escalated displays involving high costs, such as grapple and mandible flare, increased in frequency when the benefits of winning contests were high in G.bimaculatus. Escalation to grapple behaviour was less evident for males fed the lower quality diet as this imposed energy constraints on high cost displays.

Simulations magnétohydrodynamiques en régime idéal

Cette thèse s’intéresse à la modélisation magnétohydrodynamique des écoulements de fluides conducteurs d’électricité multi-échelles en mettant l’emphase sur deux applications particulières de la physique solaire: la modélisation des mécanismes des variations de l’irradiance via la simulation de la dynamo globale et la reconnexion magnétique. Les variations de l’irradiance sur les périodes des jours, des mois et du cycle solaire de 11 ans sont très bien expliquées par le passage des régions actives à la surface du Soleil. Cependant, l’origine ultime des variations se déroulant sur les périodes décadales et multi-décadales demeure un sujet controversé. En particulier, une certaine école de pensée affirme qu’une partie de ces variations à long-terme doit provenir d’une modulation de la structure thermodynamique globale de l’étoile, et que les seuls effets de surface sont incapables d’expliquer la totalité des fluctuations. Nous présentons une simulation globale de la convection solaire produisant un cycle magnétique similaire en plusieurs aspects à celui du Soleil, dans laquelle le flux thermique convectif varie en phase avec l’ ́energie magnétique. La corrélation positive entre le flux convectif et l’énergie magnétique supporte donc l’idée qu’une modulation de la structure thermodynamique puisse contribuer aux variations à long-terme de l’irradiance. Nous analysons cette simulation dans le but d’identifier le mécanisme physique responsable de la corrélation en question et pour prédire de potentiels effets observationnels résultant de la modulation structurelle. La reconnexion magnétique est au coeur du mécanisme de plusieurs phénomènes de la physique solaire dont les éruptions et les éjections de masse, et pourrait expliquer les températures extrêmes caractérisant la couronne. Une correction aux trajectoires du schéma semi-Lagrangien classique est présentée, qui est basée sur la solution à une équation aux dérivées partielles nonlinéaire du second ordre: l’équation de Monge-Ampère. Celle-ci prévient l’intersection des trajectoires et assure la stabilité numérique des simulations de reconnexion magnétique pour un cas de magnéto-fluide relaxant vers un état d’équilibre.

El costo de la atención ambulatoria del lupus eritematoso sistémico en Colombia. Contrastes y comparaciones con otras poblaciones.

Introducción: el lupus eritematoso sistémico (LES) es considerado una enfermedad de alto costo. La expresión clínica de la enfermedad depende de la ubicación geografía y la etnicidad. El objetivo de este estudio fue el calcular los costos ambulatorios relacionado al LES en una cohorte colombiana, identificar los predictores de costos y comparar nuestro resultados con otras poblaciones. Métodos: Se realizó una aproximación de tipo prevalencia en 100 pacientes LES en quienes se evaluaron los costos directos médicos, directos no médicos, indirectos e intangibles. Todos los costos médicos fueron evaluados usando una metodología abajo hacia arriba. Los costos directos fueron valorados desde una perspectiva social usando una metodología de micro-costeo. Los costos indirectos se evaluaron mediante una aproximación de capital humano, y los costos intangibles calculados a partir de los años de vida ajustados por calidad (AVAC). Se analizaron los datos por medio de un análisis multivariado. Para comparaciones con otras poblaciones todos los costos fueron expresados como la razón entre los costos y producto interno bruto nacional per cápita. Resultados: La media de costos totales fue 13.031±9.215 USD (ajustados por el factor de conversión de paridad del poder adquisitivo), lo cual representa el 1,66 del PIB per capita de Colombia. Los costos directos son el 64% de los costos totales. Los costos médicos representan el 80% de los costos directos,. Los costos indirectos fueron el 10% y los costos intangibles el 25% de los costos totales. Los medicamentos representaron el 45% de los costos directos. Mayores costos se relacionaron con el estrato socioeconómico, seguro médico privado, AVAC, alopecia, micofenolato mofetilo, y terapia anticoagulante. Los costos directos ajustados de los pacientes con LES en Colombia fueron mayores que en Norte América y en Europa. Conclusiones: el LES impone una carga económica importante para la sociedad. Los costos relacionados con la atención médica y AVAC fueron los principales contribuyentes al alto costo de la enfermedad. Estos resultados pueden ser referencia para determinar políticas en salud pública así como comparar el gasto en salud de forma internacional.

Space physics for graduate students: an activities-based approach

The geospace environment is controlled largely by events on the Sun, such as solar flares and coronal mass ejections, which generate significant geomagnetic and upper atmospheric disturbances. The study of this Sun-Earth system, which has become known as space weather, has both intrinsic scientific interest and practical applications. Adverse conditions in space can damage satellites and disrupt communications, navigation, and electric power grids, as well as endanger astronauts. The Center for Integrated Space Weather Modeling (CISM), a Science and Technology Center (STC) funded by the U.S. National Science Foundation (see http://www.bu.edu/cism/), is developing a suite of integrated physics-based computer models that describe the space environment from the Sun to the Earth for use in both research and operations [Hughes and Hudson, 2004, p. 1241]. To further this mission, advanced education and training programs sponsored by CISM encourage students to view space weather as a system that encompasses the Sun, the solar wind, the magnetosphere, and the ionosphere/thermosphere. This holds especially true for participants in the CISM space weather summer school [Simpson, 2004].

Solar induced climate effects

Solar electromagnetic radiation powers Earth’s climate system and, consequently, it is often naively assumed that changes in this solar output must be responsible for changes in Earth’s climate. However, the Sun is close to a blackbody radiator and so emits according to its surface temperature and the huge thermal time constant of the outer part of the Sun limits the variability in surface temperature and hence output. As a result, on all timescales of interest, changes in total power output are limited to small changes in effective surface temperature (associated with magnetic fields) and potential, although as yet undetected, solar radius variations. Larger variations are seen in the UV part of the spectrum which is emitted from the lower solar atmosphere (the chromosphere) and which influences Earth’s stratosphere. There is interest in“top-down” mechanisms whereby solar UV irradiance modulates stratospheric temperatures and winds which, in turn, may influence the underlying troposphere where Earth’s climate and weather reside. This contrasts with “bottom-up” effects in which the small total solar irradiance (dominated by the visible and near-IR) variations cause surface temperature changes which drive atmospheric circulations. In addition to these electromagnetic outputs, the Sun modulates energetic particle fluxes incident on the Earth. Solar Energetic Particles (SEP) are emitted by solar flares and from the shock fronts ahead of supersonic (and super-Alfvenic) ejections of material from the solar atmosphere. These SEPs enhance the destruction of polar stratospheric ozone which could be an additional form of top-down climate forcing. Even more energetic are Galactic Cosmic Rays (GCRs). These particles are not generated by the Sun, rather they originate at the shock fronts emanating from violent galactic events such as supernovae explosions; however, the expansion of the solar magnetic field into interplanetary space means that the Sun modulates the number of GCRs reaching Earth. These play a key role in enabling Earth’s global electric (thunderstorm) circuit and it has been proposed that they also modulate the formation of clouds. Both electromagnetic and corpuscular solar effects are known to vary over the solar magnetic cycle which is typically between 10 and 14 yrs in length (with an average close to 11 yrs). The solar magnetic field polarity at any one phase of one of these activity cycles is opposite to that at the same phase of the next cycle and this influences some phenomena, for example GCRs, which therefore show a 22 yr (“Hale”) cycle on average. Other phenomena, such as irradiance modulation, do not depend on the polarity of the magnetic field and so show only the basic 11-yr activity cycle. However, any effects on climate are much more significant for solar drifts over centennial timescales. This chapter discusses and evaluates potential effects on Earth’s climate system of variations in these solar inputs. Because of the great variety of proposed mechanisms, the wide range of timescales studied (from days to millennia) and the many debates (often triggered by the application of inadequate statistical methods), the literature on this subject is vast, complex, divergent and rapidly changing: consequently the number of references cited in this review is very large (yet still only a small fraction of the total).

Multiple-scattering in radar systems: a review

Although extensively studied within the lidar community, the multiple scattering phenomenon has always been considered a rare curiosity by radar meteorologists. Up to few years ago its appearance has only been associated with two- or three-body-scattering features (e.g. hail flares and mirror images) involving highly reflective surfaces. Recent atmospheric research aimed at better understanding of the water cycle and the role played by clouds and precipitation in affecting the Earth's climate has driven the deployment of high frequency radars in space. Examples are the TRMM 13.5 GHz, the CloudSat 94 GHz, the upcoming EarthCARE 94 GHz, and the GPM dual 13-35 GHz radars. These systems are able to detect the vertical distribution of hydrometeors and thus provide crucial feedbacks for radiation and climate studies. The shift towards higher frequencies increases the sensitivity to hydrometeors, improves the spatial resolution and reduces the size and weight of the radar systems. On the other hand, higher frequency radars are affected by stronger extinction, especially in the presence of large precipitating particles (e.g. raindrops or hail particles), which may eventually drive the signal below the minimum detection threshold. In such circumstances the interpretation of the radar equation via the single scattering approximation may be problematic. Errors will be large when the radiation emitted from the radar after interacting more than once with the medium still contributes substantially to the received power. This is the case if the transport mean-free-path becomes comparable with the instrument footprint (determined by the antenna beam-width and the platform altitude). This situation resembles to what has already been experienced in lidar observations, but with a predominance of wide- versus small-angle scattering events. At millimeter wavelengths, hydrometeors diffuse radiation rather isotropically compared to the visible or near infrared region where scattering is predominantly in the forward direction. A complete understanding of radiation transport modeling and data analysis methods under wide-angle multiple scattering conditions is mandatory for a correct interpretation of echoes observed by space-borne millimeter radars. This paper reviews the status of research in this field. Different numerical techniques currently implemented to account for higher order scattering are reviewed and their weaknesses and strengths highlighted. Examples of simulated radar backscattering profiles are provided with particular emphasis given to situations in which the multiple scattering contributions become comparable or overwhelm the single scattering signal. We show evidences of multiple scattering effects from air-borne and from CloudSat observations, i.e. unique signatures which cannot be explained by single scattering theory. Ideas how to identify and tackle the multiple scattering effects are discussed. Finally perspectives and suggestions for future work are outlined. This work represents a reference-guide for studies focused at modeling the radiation transport and at interpreting data from high frequency space-borne radar systems that probe highly opaque scattering media such as thick ice clouds or precipitating clouds.

A new South American network to study the atmospheric electric field and its variations related to geophysical phenomena

In this paper we present the capability of a new network of field mill sensors to monitor the atmospheric electric field at various locations in South America; we also show some early results. The main objective of the new network is to obtain the characteristic Universal Time diurnal curve of the atmospheric electric field in fair weather, known as the Carnegie curve. The Carnegie curve is closely related to the current sources flowing in the Global Atmospheric Electric Circuit so that another goal is the study of this relationship on various time scales (transient/monthly/seasonal/annual). Also, by operating this new network, we may also study departures of the Carnegie curve from its long term average value related to various solar, geophysical and atmospheric phenomena such as the solar cycle, solar flares and energetic charged particles, galactic cosmic rays, seismic activity and specific meteorological events. We then expect to have a better understanding of the influence of these phenomena on the Global Atmospheric Electric Circuit and its time-varying behavior.

Transient reconnection: Search for ionospheric signatures

The concept of magnetic reconnection originated with the suggestion by Giovanelli [1946] that particles could be energized during solar flares near nulls in the magnetic field. Hoyle [1949] subsequently proposed that such a process could also act at nulls between the geomagnetic field and the interplanetary magnetic field (IMF) to generate the energized particles responsible for auroral displays. However, the idea of the interconnection of the two magnetic fields, as we know it today, was first presented by Hoyle's student, Dungey [1953, 1961].

MAGNETOHYDRODYNAMIC SIMULATIONS OF RECONNECTION AND PARTICLE ACCELERATION: THREE-DIMENSIONAL EFFECTS

Magnetic fields can change their topology through a process known as magnetic reconnection. This process in not only important for understanding the origin and evolution of the large-scale magnetic field, but is seen as a possibly efficient particle accelerator producing cosmic rays mainly through the first-order Fermi process. In this work we study the properties of particle acceleration inserted in reconnection zones and show that the velocity component parallel to the magnetic field of test particles inserted in magnetohydrodynamic (MHD) domains of reconnection without including kinetic effects, such as pressure anisotropy, the Hall term, or anomalous effects, increases exponentially. Also, the acceleration of the perpendicular component is always possible in such models. We find that within contracting magnetic islands or current sheets the particles accelerate predominantly through the first-order Fermi process, as previously described, while outside the current sheets and islands the particles experience mostly drift acceleration due to magnetic field gradients. Considering two-dimensional MHD models without a guide field, we find that the parallel acceleration stops at some level. This saturation effect is, however, removed in the presence of an out-of-plane guide field or in three-dimensional models. Therefore, we stress the importance of the guide field and fully three-dimensional studies for a complete understanding of the process of particle acceleration in astrophysical reconnection environments.

Tomographic Simulations of accretion disks in cataclysmic variables - Flickering and wind

Both continuum and emission line flickering are phenomena directly associated with the mass-accretion process. In this work we simulated accretion-disk Doppler maps, including the effects of winds and flickering flares. Synthetic flickering Doppler maps were calculated and the effect of the flickering parameters on the maps was explored. Jets and winds occur in many astrophysical objects where accretion disks are present. Jets are generally absent among the cataclysmic variables (CVs), but there is evidence of mass loss by wind in many objects. CVs are ideal objects to study accretion disks, and consequently to study the wind associated with these disks. We also present simulations of accretion disks, including the presence of a wind with orbital phase resolution. Synthetic Ha line profiles in the optical region were obtained and their corresponding Doppler maps were calculated. The effect of the wind simulation parameters on the wind line profiles was also explored. From this study we verified that optically thick lines and/or emission by diffuse material into the primary Roche lobe are necessary to generate single peaked line profiles, often seen in CVs. The future accounting of these effects is suggested for interpreting Doppler tomography reconstructions.

Fast magnetic reconnection and energetic particle acceleration

Our numerical simulations show that the reconnection of magnetic field becomes fast in the presence of weak turbulence in the way consistent with the Lazarian and Vishniac (1999) model of fast reconnection. We trace particles within our numerical simulations and show that the particles can be efficiently accelerated via the first order Fermi acceleration. We discuss the acceleration arising from reconnection as a possible origin of the anomalous cosmic rays measured by Voyagers. (C) 2010 Elsevier Ltd. All rights reserved.

SIMULATIONS OF WINDS OF WEAK-LINED T TAURI STARS: THE MAGNETIC FIELD GEOMETRY AND THE INFLUENCE OF THE WIND ON GIANT PLANET MIGRATION

By means of numerical simulations, we investigate magnetized stellar winds of pre-main-sequence stars. In particular, we analyze under which circumstances these stars will present elongated magnetic features (e.g., helmet streamers, slingshot prominences, etc). We focus on weak-lined T Tauri stars, as the presence of the tenuous accretion disk is not expected to have strong influence on the structure of the stellar wind. We show that the plasma-beta parameter (the ratio of thermal to magnetic energy densities) is a decisive factor in defining the magnetic configuration of the stellar wind. Using initial parameters within the observed range for these stars, we show that the coronal magnetic field configuration can vary between a dipole-like configuration and a configuration with strong collimated polar lines and closed streamers at the equator (multicomponent configuration for the magnetic field). We show that elongated magnetic features will only be present if the plasma-beta parameter at the coronal base is beta(0) << 1. Using our self-consistent three-dimensional magnetohydrodynamics model, we estimate for these stellar winds the timescale of planet migration due to drag forces exerted by the stellar wind on a hot-Jupiter. In contrast to the findings of Lovelace et al., who estimated such timescales using the Weber and Davis model, our model suggests that the stellar wind of these multicomponent coronae are not expected to have significant influence on hot-Jupiters migration. Further simulations are necessary to investigate this result under more intense surface magnetic field strengths (similar to 2-3 kG) and higher coronal base densities, as well as in a tilted stellar magnetosphere.