International Research Symposium on Talent Education, Part 5: The challenges of offering group class

This is the fifth installment in a series of articles reporting on a large‐scale demographic survey of North American Suzuki teachers. The last article in this series examined some of the perceived benefits of group class. In this article, we will review participants’ perceptions of the challenges of group class. Participating teachers were asked to respond to the open‐ended question, "What is the greatest challenge of group class?" Their responses were coded and analyzed for important themes

International Research Symposium on Talent Education, Part 6: Parent education in Suzuki studios

This is the sixth installment in a series of articles reporting on a large‐scale demographic survey of North American Suzuki teachers. The previous article in this series examined some of the perceived challenges of group class. In this article, we will review teachers' descriptions of the parent education offerings within their studios. Teachers were asked to provide information about the structure, content, and intensity of their parent education programs. The survey questions included both initial education for new families entering their studios, as well as ongoing education for returning families

International Research Symposium on Talent Education, Part 4: The joys and benefits of Suzuki group class

This is the fourth article in a series reporting the findings of a large-scale demographic study of Suzuki teachers in Canada and the United States. Previous articles introduced the research, reporting on basic demographic statistics, teacher training, studio size, and structure of group classes. In this article we report on the results of an open-ended response question regarding the benefits of student participation in Suzuki group class

International Research Symposium on Talent Education, Part 3: What do Suzuki studios look like?

This is the third article in a series reporting the findings of a large-scale demographic study of 1128 North American SAA member teachers. The first article introduced the International Research Symposium on Talent Education and the group's current research interests. The second installment in the series focused on Suzuki teachers and included basic demographic information and information on teachers' training. In this article, we will explore what Suzuki studios look like, examining data such as studio size and structure of group classes

Superbubble dynamics in globular cluster infancy. I. How do globular clusters first lose their cold gas?

M. Krause1, C. Charbonnel, T. Decressin, G. Meynet, N. Prantzos, and R. Diehl, 'Superbubble dynamics in globular cluster infancy', Astronomy & Astrophysics, Vol. 546, L5 (2012), the version of record is available online at DOI: 10.1051/0004-6361/201220244. Published by EDP Sciences. © ESO 2012.The picture of the early evolution of globular clusters has been significantly revised in recent years. Current scenarios require at least two generations of stars of which the first generation (1G), and therefore also the protocluster cloud, has been much more massive than the currently predominating second generation (2G). Fast gas expulsion is thought to unbind the majority of the 1G stars. Gas expulsion is also mandatory to remove metal-enriched supernova ejecta, which are not found in the 2G stars. It has long been thought that the supernovae themselves are the agent of the gas expulsion, based on crude energetics arguments. Here, we assume that gas expulsion happens via the formation of a superbubble, and describe the kinematics by a thin-shell model. We find that supernova-driven shells are destroyed by the Rayleigh-Taylor instability before they reach escape speed for all but perhaps the least massive and most extended clusters. More power is required to expel the gas, which might plausibly be provided by a coherent onset of accretion onto the stellar remnants. The resulting kpc-sized bubbles might be observable in Faraday rotation maps with the planned Square Kilometre Array radio telescope against polarised background radio lobes if a globular cluster would happen to form in front of such a radio lobe.Peer reviewe

A New View of the Circumstellar Environment of SN 1987A

We summarize the analysis of a uniform set of both previously-known and newly-discovered scattered-light echoes, detected within 30" of SN 1987A in ten years of optical imaging, and with which we have constructed the most complete three-dimensional model of the progenitor's circumstellar environment. Surrounding the SN is a richly-structured bipolar nebula. An outer, double-lobed ``peanut,'' which we believe is the contact discontinuity between the red supergiant and main sequence winds, is a prolate shell extending 28 ly along the poles and 11 ly near the equator. Napoleon's Hat, previously believed to be an independent structure, is the waist of this peanut, which is pinched to a radius of 6 ly. Interior, the innermost circumstellar material lies along a cylindrical hourglass, 1 ly in radius and 4 ly long, which connects to the peanut by a thick equatorial disk. The nebulae are inclined 41o south and 8o east of the line of sight, slightly elliptical in cross section, and marginally offset west of the SN. The 3-D geometry of the three circumstellar rings is studied, suggesting the equatorial ring is elliptical (b/a<0.98), and spatially offset in the same direction as the hourglass. Dust-scattering models suggest that between the hourglass and bipolar lobes: the gas density drops from 1--3 cm^{-3} to >0.03 cm^{-3}; the maximum dust-grain size increases from ~0.2 micron to 2 micron; and the Si:C dust ratio decreases. The nebulae have a total mass of ~1.7 Msun, yielding a red-supergiant mass loss around 5*10^{-6} Msun yr^{-1}.Comment: Accepted for publication in ApJ 2/14/05. 16 pages in emualteapj forma

Abundance analysis of the outer halo globular cluster Palomar 14

We determine the elemental abundances of nine red giant stars belonging to Palomar 14 (Pal 14). Pal 14 is an outer halo globular cluster (GC) at a distance of \sim 70 kpc. Our abundance analysis is based on high-resolution spectra and one-dimensional stellar model atmospheres.We derived the abundances for the iron peak elements Sc, V, Cr, Mn, Co, Ni, the {\alpha}-elements O, Mg, Si, Ca, Ti, the light odd element Na, and the neutron-capture elements Y, Zr, Ba, La, Ce, Nd, Eu, Dy, and Cu. Our data do not permit us to investigate light element (i.e., O to Mg) abundance variations. The neutron-capture elements show an r-process signature. We compare our measurements with the abundance ratios of inner and other outer halo GCs, halo field stars, GCs of recognized extragalactic origin, and stars in dwarf spheroidal galaxies (dSphs). The abundance pattern of Pal 14 is almost identical to those of Pal 3 and Pal 4, the next distant members of the outer halo GC population after Pal 14. The abundance pattern of Pal 14 is also similar to those of the inner halo GCs, halo field stars, and GCs of recognized extragalactic origin, but differs from what is customarily found in dSphs field stars. The abundance properties of Pal 14 as well as those of the other outer halo GCs are thus compatible with an accretion origin from dSphs. Whether or not GC accretion played a role, it seems that the formation conditions of outer halo GCs and GCs in dSphs were similar.Comment: 19 pages, 15 figures. Accepted by A&

Social approach in genetically engineered mouse lines relevant to autism

Profound impairment in social interaction is a core symptom of autism, a severe neurodevelopmental disorder. Deficits can include a lack of interest in social contact and low levels of approach and proximity to other children. In this study, a three-chambered choice task was used to evaluate sociability and social novelty preference in five lines of mice with mutations in genes implicated in autism spectrum disorders. Fmr1tm1Cgr/Y (Fmr1−/y) mice represent a model for fragile X, a mental retardation syndrome that is partially co-morbid with autism. We tested Fmr1−/y mice on two genetic backgrounds, C57BL/6J and FVB/N-129/OlaHsd (FVB/129). Targeted disruption of Fmr1 resulted in low sociability on one measure, but only when the mutation was expressed on FVB/129. Autism has been associated with altered serotonin levels and polymorphisms in SLC6A4 (SERT), the serotonin-transporter gene. Male mice with targeted disruption of Slc6a4 displayed significantly less sociability than wildtype controls. Mice with conditional overexpression of Igf-1 (Insulin-like growth factor-1) offered a model for brain overgrowth associated with autism. Igf-1 transgenic mice engaged in levels of social approach similar to wildtype controls. Targeted disruption in other genes of interest, En2 (Engrailed 2) and Dhcr7, was carried on genetic backgrounds that demonstrated low levels of exploration in the choice task, precluding meaningful interpretations of social behavior scores. Overall, results show that loss of Fmr1 or Slc6a4 gene function can lead to deficits in sociability. Findings from the fragile X-model suggest that the FVB/129 background confers enhanced susceptibility to consequences of Fmr1 mutation on social approach

Dynamical Processes in Globular Clusters

Globular clusters are among the most congested stellar systems in the Universe. Internal dynamical evolution drives them toward states of high central density, while simultaneously concentrating the most massive stars and binary systems in their cores. As a result, these clusters are expected to be sites of frequent close encounters and physical collisions between stars and binaries, making them efficient factories for the production of interesting and observable astrophysical exotica. I describe some elements of the competition among stellar dynamics, stellar evolution, and other processes that control globular cluster dynamics, with particular emphasis on pathways that may lead to the formation of blue stragglers.Comment: Chapter 10, in Ecology of Blue Straggler Stars, H.M.J. Boffin, G. Carraro & G. Beccari (Eds), Astrophysics and Space Science Library, Springe