Coronal winds powered by radiative driving

A two-component phenomenological model developed originally for zeta Puppis is revised in order to model the outflows of late-type O dwarfs that exhibit the weak-wind phenomenon. With the theory's standard parameters for a generic weak-wind star, the ambient gas is heated to coronal temperatures ~ 3 x 10^{6}K at radii > 1.4 R, with cool radiativly-driven gas being then confined to dense clumps with filling factor ~ 0.02. Radiative driving ceases at radius ~ 2.1R when the clumps are finally destroyed by heat conduction from the coronal gas. Thereafter, the outflow is a pure coronal wind, which cools and decelerates reaching infinity with terminal velocity ~ 980$ km/ s.Comment: 10 pages, 4 figure

Colonial Privileges in a Settler Society: Disparities of Cultural Capital in a University Setting

Drawing on forty one-on-one interviews with third year students from The University of Auckland, this study contrasts the experiences of students from working- and upper-class backgrounds. In particular, the study demonstrates how working-class students, most of whom come from Indigenous Māori and Pacific ethnic backgrounds, are forced to navigate obstacles infused with interpersonal and institutional racism. These students also report a stigmatising awareness of their lack of privilege and sense of obligation to give back to their ethnic communities. In contrast students from upper-class backgrounds, though hard-working, discuss a litany of opportunities extending their academic and occupational privilege. These capital-building opportunities are tightly connected to consistent family support in the form of gifted money, flexible work options, and networks that enhance professional experience. Working with kaupapa Māori and Bourdeausian conceptual frameworks, the study highlights privileged students’ ability to access and extend their objectified cultural capital, as less economically privileged students work their way through colonial blockades and classed pitfalls. Given the clear disparities expressed by study participants, the research suggests universities radically reframe how resources are allocated to students from diverse backgrounds

My body until proven otherwise: Exploring the time course of the full body illusion

Evidence from the Full Body Illusion (FBI) has shown that adults can embody full bodies which are not their own when they move synchronously with their own body or are viewed from a first-person perspective. However, there is currently no consensus regarding the time course of the illusion. Here, for the first time, we examined the effect of visuomotor synchrony (synchronous/asynchronous/no movement) on the FBI over time. Surprisingly, we found evidence of embodiment over a virtual body after five seconds in all conditions. Embodiment decreased with increased exposure to asynchronous movement, but remained high in synchronous and no movement conditions. We suggest that embodiment of a body seen from a first-person perspective is felt by default, and that embodiment can then be lost in the face of contradictory cues. These results have significant implications for our understanding of how multisensory cues contribute to embodiment

Physical properties and small-scale structure of the Lyman-alpha forest: Inversion of the HE 1122-1628 UVES spectrum

We study the physical properties of the Lyman-alpha forest by applying the inversion method described by Pichon et al. (2001) to the high resolution and high S/N ratio spectrum of the z_em=2.40 quasar HE 1122-1628 obtained during Science Verification of UVES at the VLT. We compare the column densities obtained with the new fitting procedure with those derived using standard Voigt profile methods. The agreement is good and gives confidence in the new description of the Lyman-alpha forest as a continuous field as derived from our method. We show that the observed number density of lines with logN>13 and 14 is, respectively, 50 and 250 per unit redshift at z~2. We study the physical state of the gas, neglecting peculiar velocities, assuming a relation between the overdensity and the temperature. T=Tbar * rho^(2beta). There is an intrinsic degeneracy between the parameters beta and Tbar. We demonstrate that, at a fixed beta, the temperature at mean density, Tbar, can be uniquely extracted however. While applying the method to HE 1122-1628, we conclude that for 0.2<beta<0.3, 6000<Tbar<15000 K at z~2. We investigate the small scale structure of strong absorption lines using the information derived from the Lyman-beta, Lyman-gamma and Civ profiles. Introducing the Lyman-beta line in the fit allows us to reconstruct the density field up to rho~10 instead of 5 for the Lyman-alpha line only. There may be small velocity shifts ~10km.s^{-1} between the peaks in the Civ and Hi density profiles. Although the statistics is small, it seems that Civ/Hi and n_HI are anti-correlated. This could be a consequence of the high sensitivity of the Civ/Hi ratio to temperature. The presence of associated Ovi absorption, with similar profile, confirms that the gas is photo-ionized and at a temperature of T~10^5 K.Comment: 15 pages, 21 figures, accepted for publication in A&A. Quoted results from other papers in section 4.2 have been modifie

Simulating the formation and evolution of galaxies: Multi-phase description of the interstellar medium, star formation, and energy feedback

We present a multi-phase representation of the ISM in NB-TSPH simulations of galaxy formation and evolution with particular attention to the case of early-type galaxies. Cold gas clouds are described by the so-called sticky particles algorithm. They can freely move throughout the hot ISM medium; stars form within these clouds and the mass exchange among the three baryonic phases (hot gas, cold clouds, stars) is governed by radiative and Compton cooling and energy feedback by supernova (SN) explosions, stellar winds, and UV radiation. We also consider thermal conduction, cloud-cloud collisions, and chemical enrichment. Our model agrees with and improves upon previous studies on the same subject. The results for the star formation rate are very promising and agree with recent observational data on early-type galaxies. These models lend further support to the revised monolithic scheme of galaxy formation, which has recently been also strengthened by high redshift data leading to the so-called downsizing and top-down scenarios.Comment: 17 pages, 17 figure

Management of Skin Toxicity Related to the Use of Imatinib Mesylate (STI571, Glivec™) for Advanced Stage Gastrointestinal Stromal Tumours

Skin toxicity is a common side-effect of treatment with imatinib mesylate (STI571, Glivec™) in advanced gastrointestinal stromal tumours (GIST) and chronic myeloid leukaemia. The optimal duration of treatment with imatinib mesylate in GIST has not yet been established, as durable remissions have been observed in patients. It is, therefore, important to develop strategies to deal with common side-effects of what may be a long-term treatment. Here we report the case of a patient with advanced GIST who developed a cutaneous drug reaction secondary to imatinib mesylate and the various management options that may be employed depending upon the severity of the toxicity. The case and literature are discussed

Differences in Hemoglobin A 1c Between Hispanics/Latinos and Non-Hispanic Whites: An Analysis of the Hispanic Community Health Study/Study of Latinos and the 2007–2012 National Health and Nutrition Examination Survey

To determine whether, after adjustment for glycemia and other selected covariates, hemoglobin A1c (HbA1c) differed among adults from six Hispanic/Latino heritage groups (Central American, Cuban, Dominican, Mexican, Puerto Rican, and South American) and between Hispanic/Latino and non-Hispanic white adults without self-reported diabetes

Cosmological simulations of the high-redshift radio universe

Using self-consistent cosmological simulations of disc galaxy formation, we analyse the 1.4 GHz radio flux from high-redshift progenitors of present-day normal spirals within the context of present-day and planned next-generation observational facilities. We demonstrate that while current radio facilities such as the Very Large Array (VLA) are unlikely to trace these progenitors beyond redshifts z<0.2, future facilities such as the Square Kilometer Array (SKA) will readily probe their characteristics to redshifts z<2, and are likely to provide detections beyond z~3. We also demonstrate that the progenitors of present-day cD galaxies can emit in excess of 10 uJy of flux at redshifts z>1, and may be a non-negligible contributor to the micro-Jansky source counts derived from current deep VLA cm-wave surveys.Comment: 7 pages, 5 figures, accepted for publication in MNRAS. High resolution version is available at http://astronomy.swin.edu.au/staff/dkawata/research/papers.htm

Thermal conduction in cosmological SPH simulations

Thermal conduction in the intracluster medium has been proposed as a possible heating mechanism for offsetting central cooling losses in rich clusters of galaxies. In this study, we introduce a new formalism to model conduction in a diffuse ionised plasma using smoothed particle hydrodynamics (SPH), and we implement it in the parallel TreePM/SPH-code GADGET-2. We consider only isotropic conduction and assume that magnetic suppression can be described in terms of an effective conductivity, taken as a fixed fraction of the temperature-dependent Spitzer rate. We also account for saturation effects in low-density gas. Our formulation manifestly conserves thermal energy even for individual and adaptive timesteps, and is stable in the presence of small-scale temperature noise. This allows us to evolve the thermal diffusion equation with an explicit time integration scheme along with the ordinary hydrodynamics. We use a series of simple test problems to demonstrate the robustness and accuracy of our method. We then apply our code to spherically symmetric realizations of clusters, constructed under the assumptions of hydrostatic equilibrium and a local balance between conduction and radiative cooling. While we confirm that conduction can efficiently suppress cooling flows for an extended period of time in these isolated systems, we do not find a similarly strong effect in a first set of clusters formed in self-consistent cosmological simulations. However, their temperature profiles are significantly altered by conduction, as is the X-ray luminosity.Comment: 14 pages, 7 figures, accepted by MNRAS, high resolution version available at http://www.mpa-garching.mpg.de/~jubelgas/conduction.pdf. Fixed typos in eq. 20,22,2