The Blacksmith Blues / music by Jack Holmes; words by Jack Holmes

Cover: photo of singer Ella Mae Morse; Publisher: Hill and Range Songs Inc. (Beverly Hills)https://egrove.olemiss.edu/sharris_e/1081/thumbnail.jp

On the process of accretion in the formation of the planets and comets

The physically reasonable assumption that the seed bodies which initiated the accretion of the individual asteroids, planets, and comets (subsequently these objects are collectively called planetoids) formed by stochastic processes requires a radius distribution function which is unique except for two scaling parameters: the total number of planetoids and their most probable radius. The former depends on the ease of formation of the seed bodies while the second is uniquely determined by the average pre-encounter velocity, V, of the accretable material relative to an individual planetoid. This theoretical radius function can be fit to the initial asteroid radius distribution which [Anders, 1965] derived from the present-day distribution by allowing for fragmentation collisions among the asteroids since their formation. Normalizing the theoretical function to this empirical distribution reveals that there were about 102 precollision asteroids and that V = (2-4) x 10-2 km/sec which was presumably the turbulent velocity in the Solar Nebula. Knowing V we can determine the scale height of the dust in the Solar Nebula and consequently its space density. The density of accretable material determines the rate of accretion of the planetoids. From this we find, for example, that the Earth formed in about 8 x 106 yr and it attained a maximum temperature through accretion of about 3 x 103[deg]K. From the total mass of the terrestrial planets and the theoretical radius function we find that about 2 x 103 planetoids formed in the vicinity of the terrestrial planets. Except for the asteroids the smaller planetoids have since been accreted by the terrestrial planets. About 15% of the present mass of the terrestrial planets was accumulated by the secondary accretion of these smaller primary planetoids. There are far fewer primary planetoids than craters on the Moon or Mars. The craters were likely produced by the collisional breakup of a few primary planetoids with masses between one-tenth and one lunar mass. This deduction comes from comparing the collision cross sections of the planetoids in this mass range to that of the terrestrial planets. This comparison shows that two to three collisions leading to the breakup of four to six objects likely occurred among these objects before their accretion by the terrestrial planets. The number of these fragments is quite adequate to explain the lunar and Martin craters. Furthermore the mass spectrum of such fragments is a power-law distribution which results in a power-law distribution of crater radii of just the type observed on the Moon and Mars. Applying the same analysis to the planetoids which formed in the vicinity of the giant planets reveals that it is unlikely that any fragmentation collisions took place among them before they were accreted by these planets due to the integrated collision cross section of the giant planets being about three orders of magnitude greater than that of the terrestrial planets. We can thus anticipate a marked scarcity of impact craters on the satellites of these outer planets. This prediction can be tested by future space probes. Our knowledge of the radius function of the comets is consistent with their being primary planetoids. The primary difference between the radius function of the planetoids which formed in the inner part of the solar system and that of the comets results from the fact that the seed bodies which grew into the comets formed far more easily than those which grew into the asteroids and the terrestrial planets. Thus in the outer part of the Solar Nebula the principal solid material (water and ammonia snow) accreted into a huge (~1012+) number of relatively small objects (comets) while in the inner part of the nebula the solid material (hard-to-stick refractory substances) accumulated into only a few (~103) large objects (asteroids and terrestrial planets). Uranus and Neptune presumably formed by the secondary accretion of the comets.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/33936/1/0000203.pd

NHS North Central London clinical commissioning group winter resilience communications and engagement campaign 2021/2022. Evaluation report

This evaluation study was commissioned by the Communications and Engagement team at the NHS North Central London Clinical Commissioning Group to assess the performance of the Winter Resilience Communications and Engagement campaign during the months of December 2021 and March 2022. The campaign aimed to deliver ‘an integrated system-wide communications and engagement programme to support residents, patients and health and care workers prepare for, and stay well this winter, reminding them that services are open and ready to provide care when needed and to access care in the right place at the right time’ (NCL CCG, 2021). The evaluation was conducted following the Evaluation Framework 2.0, with metrics for the 3 components of the Winter resilience campaign which sought to raise awareness, change behaviour intentions, and effect behaviour change. A mixed-methods complementarity study was used, combining quantitative and qualitative methods of data collection and analysis. We envision a three-stage process: 1) A baseline survey used as the control; 2) a modify repeat survey (post-campaign); 3) one-to-one interviews with staff involved in the delivery and with respondents to the final survey. Contextual data from NHS digital and GOV.UK were used to strengthen the evidence for the evaluation analysis. The evaluation makes recommendations directly relevant to the Communications and Engagement team as they prepare for the next Winter campaign. Recommendations focus on two main areas, campaign preparation and content, the latter is mapped against a diagnosis of behavioural components using the COM-B theoretical model and interventions informed by the Behaviour Change Wheel

Gene Banks, Seed Libraries, and Vegetable Sanctuaries: The Cultivation and Conservation of Heritage Vegetables in Britain, 1970–1985

Individual seed saving and exchange are considered important components of contemporary efforts to conserve crop genetic diversity, which ramify at local, regional, and global scales. Yet the very fact that the contributions of these activities to conservation need to be made explicit by seed savers and those who study them indicates that the practices of seed saving and exchange may not immediately be recognized as conservation-oriented activities. This article investigates why and how individual seed saving came to be aligned with a broader conservation agenda in Britain through an historical examination of the promotion of seed saving by the Henry Doubleday Research Association (HDRA) in the 1970s and 1980s. It demonstrates how several HDRA initiatives that aimed to preserve vegetable diversity also re-inscribed British gardeners' ordinary labor as conservation work. This historical study complements sociological and ethnographic studies, highlighting the role of a prominent organization in creating pathways for individuals to engage in local, national, and international conservation through seed saving. It also serves as a reminder that the connections between these activities had to be made explicit—that is, that there was (and is) work involved in connecting individual acts of seed saving to conservation outcomes at different scales

Prompt Optical Observations of Gamma-ray Bursts

The Robotic Optical Transient Search Experiment (ROTSE) seeks to measure simultaneous and early afterglow optical emission from gamma-ray bursts (GRBs). A search for optical counterparts to six GRBs with localization errors of 1 square degree or better produced no detections. The earliest limiting sensitivity is m(ROTSE) > 13.1 at 10.85 seconds (5 second exposure) after the gamma-ray rise, and the best limit is m(ROTSE) > 16.0 at 62 minutes (897 second exposure). These are the most stringent limits obtained for GRB optical counterpart brightness in the first hour after the burst. Consideration of the gamma-ray fluence and peak flux for these bursts and for GRB990123 indicates that there is not a strong positive correlation between optical flux and gamma-ray emission.Comment: 4 pages, 3 figures, submitted to ApJ Letter

Sources and Secondary Production of Organic Aerosols in the Northeastern United States during WINTER

Most intensive field studies investigating aerosols have been conducted in summer, and thus, wintertime aerosol sources and chemistry are comparatively poorly understood. An aerosol mass spectrometer was flown on the National Science Foundation/National Center for Atmospheric Research C‐130 during the Wintertime INvestigation of Transport, Emissions, and Reactivity (WINTER) 2015 campaign in the northeast United States. The fraction of boundary layer submicron aerosol that was organic aerosol (OA) was about a factor of 2 smaller than during a 2011 summertime study in a similar region. However, the OA measured in WINTER was almost as oxidized as OA measured in several other studies in warmer months of the year. Fifty‐eight percent of the OA was oxygenated (secondary), and 42% was primary (POA). Biomass burning OA (likely from residential heating) was ubiquitous and accounted for 33% of the OA mass. Using nonvolatile POA, one of two default secondary OA (SOA) formulations in GEOS‐Chem (v10‐01) shows very large underpredictions of SOA and O/C (5×) and overprediction of POA (2×). We strongly recommend against using that formulation in future studies. Semivolatile POA, an alternative default in GEOS‐Chem, or a simplified parameterization (SIMPLE) were closer to the observations, although still with substantial differences. A case study of urban outflow from metropolitan New York City showed a consistent amount and normalized rate of added OA mass (due to SOA formation) compared to summer studies, although proceeding more slowly due to lower OH concentrations. A box model and SIMPLE perform similarly for WINTER as for Los Angeles, with an underprediction at ages \u3c6 hr, suggesting that fast chemistry might be missing from the models

Lateral presentation alters overall viewing strategy

Eye tracking has been used during face categorisation and identification tasks to identify perceptually salient facial features and infer underlying cognitive processes. However, viewing patterns are influenced by a variety of gaze biases, drawing fixations to the centre of a screen and horizontally to the left side of face images (left-gaze bias). In order to investigate potential interactions between gaze biases uniquely associated with facial expression processing, and those associated with screen location, face stimuli were presented in three possible screen positions to the left, right and centre. Comparisons of fixations between screen locations highlight a significant impact of the screen centre bias, pulling fixations towards the centre of the screen and modifying gaze biases generally observed during facial categorisation tasks. A left horizontal bias for fixations was found to be independent of screen position but interacting with screen centre bias, drawing fixations to the left hemi-face rather than just to the left of the screen. Implications for eye tracking studies utilising centrally presented faces are discussed

ER and HER2 expression are positively correlated in HER2 non-overexpressing breast cancer

PMCID: PMC3446380This is an open access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/2.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited

The ROTSE detection of early optical light from GRB 990123

An overview is given of the Robotic Optical Transient Search Experiment, a ground-based observational astronomy project intended to detect visible radiation from gamma-ray bursts. The major result of the project was the detection of an early bright optical transient from a GRB. (AIP) © 1999 American Institute of Physics.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87569/2/82_1.pd