In the Archives of Compositionoffers new and revisionary narratives of composition and rhetoric's history. It examines composition instruction and practice at secondary schools and normal colleges, ...the two institutions that trained the majority of U.S. composition teachers and students during the nineteenth and twentieth centuries. Drawing from a broad array of archival and documentary sources, the contributors provide accounts of writing instruction within contexts often overlooked by current historical scholarship. Topics range from the efforts of young women to attain rhetorical skills in an antebellum academy, to the self-reflections of Harvard University students on their writing skills in the 1890s, to a close reading of a high school girl's diary in the 1960s that offers a new perspective on curriculum debates of this period. Taken together, the chapters begin to recover how high school students, composition teachers, and English education programs responded to institutional and local influences, political movements, and pedagogical innovations over a one-hundred-and-thirty-year span.
Abstract
The compositions of stars and planets are connected, but the definition of “habitability” and the “habitable zone” only take into account the physical relationship between the star and ...planet. Planets, however, are made truly habitable by both chemical and physical processes that regulate climatic and geochemical cycling between atmosphere, surface, and interior reservoirs. Despite this, an “Earth-like” planet is often defined as a planet made of a mixture of rock and Fe that is roughly 1 Earth-density. To understand the interior of a terrestrial planet, the stellar abundances of planet-building elements (e.g., Mg, Si, and Fe) can be used as a proxy for the planet’s composition. We explore the planetary mineralogy and structure for fictive planets around the 10 stars closest to the Sun using stellar abundances from the Hypatia Catalog. Although our sample contains stars that are both sub- and super-solar in their abundances, we find that the mineralogies are very similar for all 10 planets—since the error or spread in the stellar abundances create significant degeneracy in the models. We show that abundance uncertainties need to be on the order of Fe/H < 0.02 dex, Si/H < 0.01 dex, Al/H < 0.002 dex, while Mg/H and Ca/H < 0.001 dex in order to distinguish two unique planetary populations in our sample of 10 stars. While these precisions are high, we believe that they are possible given certain abundance techniques, in addition to methodological transparency, that have recently been demonstrated in the literature. However, without these precisions, the uncertainty in planetary structures will be so high that we will be unable to confidently state that a planet is like the Earth, or unlike anything we have ever seen.
The present-day envelope of gaseous planets is a relic of how these giant planets originated and evolved. Measuring their elemental composition therefore presents a powerful opportunity to answer ...long-standing questions regarding planet formation. Obtaining precise observational constraints on the elemental inventory of giant exoplanets has, however, remained challenging owing to the limited simultaneous wavelength coverage of current space-based instruments. Here, we present thermal emission observations of the nontransiting hot Jupiter τ Boo b using the new wide wavelength coverage (0.95–2.50 μm) and high spectral resolution (R = 70,000) CFHT/SPIRou spectrograph. By combining a total of 20 hr of SPIRou data obtained over five nights in a full atmospheric retrieval framework designed for high-resolution data, we constrain the abundances of all the major oxygen- and carbon-bearing molecules and recover a noninverted temperature structure using a new free-shape, nonparametric temperature–pressure profile retrieval approach. We find a volume mixing ratio of log(CO) = −\({2.46}_{-0.29}^{+0.25}\) and a highly depleted water abundance of less than 0.0072 times the expected value for a solar composition envelope. Combined with upper limits on the abundances of CH4, CO2, HCN, TiO, and C2H2, this results in a gas-phase C/H ratio of \({5.85}_{-2.82}^{+4.44}\) × solar, consistent with the value of Jupiter, and an envelope C/O ratio robustly greater than 0.60, even when taking into account the oxygen that may be sequestered out of the gas phase. Combined, the inferred supersolar C/H, O/H, and C/O ratios on τ Boo b support a formation scenario beyond the water snowline in a disk enriched in CO owing to pebble drift.
Background: Three-dimensional optical (3DO) body composition (BC) from statistical shape models have been developed and vali- dated on cross-sectional data. This technique has shown to be ac- curate ...and precise in respect to dual-energy X-ray absorptiometry (DXA). However, it is unknown if 3DO is sensitive enough to detect change in BC. Therefore, our objective was to evaluate the accuracy of the previously developed cross-sectional models for detecting change and the need for new longitudinal models. Methods: Data from participants in the longitudinal arm of the Shape Up! Adults, FB4 Study, and Louisiana State University Athlete's Study were used in this analysis. Measures on all partici- pants included 3DO and DXA scans at baseline and follow-up using similar make and model systems. Healthy participants went through study-specific interventions that included either dietary or physical activity modifications. Fat mass (FM) and visceral adipose tissue (VAT) were estimated from 3DO scans using previously-developed statistical shape models. Changes in these estimates were compared to criterion changes in DXA. Further, fundamental studies relating change in shape and demographics to DXA were performed using step-forward linear regression with 5-fold cross-validation. Results: For this analysis, 107 participants completed the study (males = 67). Of the models created, 3DO estimates of FM from the previ- ously developed cross-sectional model performed the best for females (R2 = 0.88, RMSE = 1.29 kg) while fundamental models of change in shape were best for males (R2 = 0.88, RMSE = 1.8 kg). Change in DXA VAT for both males and females was best predicted by change in shape models (R2 = 0.57 and 0.49, RMSE = 85 g and 76 g, respectively). Conclusions: Using a diverse population of healthy males and females, various 3DO models accurately estimated changes in DXA FM and VAT over time.
•The macronutrient composition of rice protein ingredients was characterised.•The mineral and amino acid composition of the ingredients was analysed.•The protein profile of the ingredients was ...investigated.•A reducing buffer was developed to solubilise rice proteins prior to SDS-PAGE.•Rice protein fractions were extracted from rice flour and characterised by SDS-PAGE.
The objective of this study was to investigate the nutrient composition and protein profile of a range of rice protein ingredients containing 32–78% total protein. Rice protein ingredients had significantly (P<0.05) lower levels of calcium and total essential amino acids compared to selected dairy protein ingredients, i.e., skim milk powder, whey protein isolate and whey protein hydrolysate. Protein profiles of the ingredients were determined by sodium dodecyl sulfate-polyacrylamide gel electrophoresis (SDS-PAGE) and size exclusion-high pressure liquid chromatography (SE-HPLC). Since the dominant rice protein fraction (i.e., glutelin) is extensively aggregated and crosslinked through disulfide bonds, a strong reducing buffer was developed in order to solubilise the rice protein ingredients prior to analysis by SDS-PAGE. Intact rice protein ingredients (n=3) contained proteins with molecular weight (MW) ranging from ∼11 to >250kDa, while rice protein hydrolysates (n=4) were composed mainly of low MW peptides. In parallel, enriched protein fractions were extracted from defatted rice flour based on their solubility and characterised by SDS-PAGE to facilitate the identification of protein bands in the rice protein ingredients. The results of this study underpin the understanding, prediction and control of physicochemical functionality of rice protein ingredients.
This book argues for the value of digital literacy in the multilingual writing classroom. Against the background of huge changes in literacy practices prompted by online communication, and a growing ...acceptance of a broader definition of academic literacy that encompasses multimodality, the book examines the relationship between digital and print literacies and addresses the design of literacy spaces for multilingual classrooms. The author critically evaluates the latest developments in the use of technology in multilingual writing spaces, and focuses on the role of teachers in their design; it also addresses areas that are not often discussed in relation to multilingual students, from blogging to publishing and intellectual property. The book will help teachers meet the challenges created by rapidly shifting technology, as well as making an innovative contribution to research on multilingual writing classrooms.
Good writing begins with good reading. This book is written on the premise that students must embrace reading as a part of the full process of good writing. It may be used by classroom teachers ...(Grades 6-12) individually or collectively as members of a professional learning community, by pre-service teachers in a literacy course, or by other educators working to support literacy in the classroom. Interdisciplinary discussions relate to all types or genres of reading and writing. This book offers practical lessons and ideas for teaching and motivating all learners using Universal Design for Learning principles. Formatting provides additional ideas for challenged students, including students with special needs, accelerated learners, and English Language Learners, and is aligned with Common Core State Standards for content subjects as well as for language arts. It takes ideas that were formerly reserved for the upper echelon of students in English language arts and reformulates teaching approaches to reach students across the learning spectrum and in all disciplines. All teachers need to be involved in raising the literacy bar, and this book provides activities and strategies for use in the classroom that can promote success for all learners.
We reevaluate the systematics and geologic setting of terrestrial, lunar, Martian, and asteroidal “impactites” resulting from single or multiple impacts. For impactites derived from silicate rocks ...and sediments, we propose a unified and updated system of progressive shock metamorphism. “Shock‐metamorphosed rocks” occur as lithic clasts or melt particles in proximal impactites at impact craters, and rarely in distal impactites. They represent a wide range of metamorphism, typically ranging from unshocked to shock melted. As the degree of shock metamorphism, at a given shock pressure, depends primarily on the mineralogical composition and the porosity of a rock or sediment sample, different shock classification systems are required for different types of planetary rocks and sediments. We define shock classification systems for eight rock and sediment classes which are assigned to three major groups of rocks and sediments (1) crystalline rocks with classes F, M, A, and U; (2) chondritic rocks (class C); and (3) sedimentary rocks and sediments with classes SR, SE, and RE. The abbreviations stand for felsic (F), mafic (M), anorthositic (A), ultramafic (U), sedimentary rocks (SR), unconsolidated sediments (SE), and regoliths (RE). In each class, the progressive stages of shock metamorphism are denominated S1 to Sx. These progressive shock stages are introduced as: S1–S7 for F, S1–S7 for M, S1–S6 for A, S1–S7 for U, S1–S7 for C, S1–S7 for SR, S1–S5 for SE, and S1–S6 for RE. S1 stands for “unshocked” and Sx (variable between S5 and S7) stands for “whole rock melting.” We propose a sequence of symbols characterizing the degree of shock metamorphism of a sample, i.e., F‐S1 to F‐S7 with the option to add the tabulated pressure ranges (in GPa) in parentheses.
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