Amas autorizadas : formação e cuidado

Dissertação de mestrado, Educação e Formação (Área de Especialidade em Organização e Gestão da Educação e da Formação), Universidade de Lisboa, Instituto de Educação, 2022Este estudo pretende investigar as competências utilizadas pelas amas autorizadas em sua prática profissional. Partiu-se da premissa que ama é uma pessoa que cuida de crianças de outras famílias, em sua própria residência, mediante pagamento e cumpre com requisitos legais, que lhe autorizam a realizar tal atividade. Foram entrevistadas sete amas autorizadas para o exercício profissional, em mais de dez horas de gravações, sendo quatro amas de creches familiares, duas amas independentes e uma ama que trabalha diretamente para o Instituto da Segurança Social I.P. Utilizando uma metodologia qualitativa, investiga-se a formação das amas e as relações com o seu fazer cotidiano. Procura-se saber mais sobre o fenômeno a partir de seu contexto, sem isolar quaisquer dos elementos investigados. Os resultados da pesquisa revelam que há diferenças importantes nas amas que possuem formação inicial. Elas estão mais alinhadas com as indicações científicas para o cuidado respeitoso e gentil (Appel & David, 2021; Montessori; 2014, 2017; Pikler, 2018; Tardos, 2014; Tonucci, 1997, 2015, 2018a) em termos de compreensão sobre as crianças e consequentemente a sua forma de orientá-las e oportunizar situações de aprendizado na vida cotidiana. As amas apresentam potencial para serem mais do que uma saída para a falta de vagas nas creches regulares, elas representam uma filosofia de cuidado!This study intends to investigate the skills used by childminders in their professional practice. It started from the premise that childminders are individuals that take care of children from other families, in their own home, against payment and fulfils legal requirements, which authorize them to conduct such activity. Seven authorized childminders for professional practice were interviewed, with more than ten hours of recordings, including four childminders from family day care, two independent childminders, and one childminder who works directly for the Social Security Institute. It uses a qualitative methodology, which investigates the learning path of childminders and the relationships with their daily activities. We aim to know more about the phenomenon from its context, without isolating any of the investigated elements. The survey results reveal that there are important differences in childminders who have initial training. They are more in line with scientific guidelines of respectful and gentle care (Appel & David, 2021; Montessori; 2014, 2017; Pikler, 2018; Tardos, 2014; Tonucci, 1997, 2015, 2018a) understanding about children and consequently their way of guiding them and providing opportunities for learning situations in everyday life. Childminders have potential to be more than a solution to the lack of places in nursery, they represent a philosophy of care

Why Economics Does Not An Ethics Make: A Case Study

This essay is a multidisciplinary case study of environmental injustice. It demonstrates that misuse of the environment can ultimately impact humans unjustly and further that attempts to remediate injustice in one area merely shifts the burden of injustice to others. After providing the historical, sociological and scientific facts surrounding the 50-acre site, an ethical assessment is presented. It was determined that the actors in this case study were not employing any ethical valuing in their decision making process, but rather relied upon economic values to make their choices. The authors then suggest that judging them from within their own economic valuing system that the actors’ decisions had failed to meet their own values, i.e. good economics

Characteristics of Kepler Planetary Candidates Based on the First Data Set: The Majority are Found to be Neptune-Size and Smaller

In the spring of 2009, the Kepler Mission commenced high-precision photometry on nearly 156,000 stars to determine the frequency and characteristics of small exoplanets, conduct a guest observer program, and obtain asteroseismic data on a wide variety of stars. On 15 June 2010 the Kepler Mission released data from the first quarter of observations. At the time of this publication, 706 stars from this first data set have exoplanet candidates with sizes from as small as that of the Earth to larger than that of Jupiter. Here we give the identity and characteristics of 306 released stars with planetary candidates. Data for the remaining 400 stars with planetary candidates will be released in February 2011. Over half the candidates on the released list have radii less than half that of Jupiter. The released stars include five possible multi-planet systems. One of these has two Neptune-size (2.3 and 2.5 Earth-radius) candidates with near-resonant periods.Comment: Paper to accompany Kepler's June 15, 2010 data release; submitted to Astrophysical Journal Figures 1,2,& 3 revised. Improved labeling on all figures. Slight changes to planet frequencies in result

Planet Occurrence within 0.25 AU of Solar-type Stars from Kepler

We report the distribution of planets as a function of planet radius (R_p), orbital period (P), and stellar effective temperature (Teff) for P < 50 day orbits around GK stars. These results are based on the 1,235 planets (formally "planet candidates") from the Kepler mission that include a nearly complete set of detected planets as small as 2 Earth radii (Re). For each of the 156,000 target stars we assess the detectability of planets as a function of R_p and P. We also correct for the geometric probability of transit, R*/a. We consider first stars within the "solar subset" having Teff = 4100-6100 K, logg = 4.0-4.9, and Kepler magnitude Kp < 15 mag. We include only those stars having noise low enough to permit detection of planets down to 2 Re. We count planets in small domains of R_p and P and divide by the included target stars to calculate planet occurrence in each domain. Occurrence of planets varies by more than three orders of magnitude and increases substantially down to the smallest radius (2 Re) and out to the longest orbital period (50 days, ~0.25 AU) in our study. For P < 50 days, the radius distribution is given by a power law, df/dlogR= k R^\alpha. This rapid increase in planet occurrence with decreasing planet size agrees with core-accretion, but disagrees with population synthesis models. We fit occurrence as a function of P to a power law model with an exponential cutoff below a critical period P_0. For smaller planets, P_0 has larger values, suggesting that the "parking distance" for migrating planets moves outward with decreasing planet size. We also measured planet occurrence over Teff = 3600-7100 K, spanning M0 to F2 dwarfs. The occurrence of 2-4 Re planets in the Kepler field increases with decreasing Teff, making these small planets seven times more abundant around cool stars than the hottest stars in our sample. [abridged]Comment: Submitted to ApJ, 22 pages, 10 figure

Masses, radii, and orbits of small Kepler planets : The transition from gaseous to rocky planets

We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm-3, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than 2 R ⊕. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O).Peer reviewedFinal Accepted Versio

2020 American College of Rheumatology Guideline for the Management of Reproductive Health in Rheumatic and Musculoskeletal Diseases

Peer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/154675/1/art41191.pdfhttps://deepblue.lib.umich.edu/bitstream/2027.42/154675/2/art41191_am.pd

A Bayesian view of murine seminal cytokine networks

It has long been established that active agents in seminal fluid are key to initiating and coordinating mating-induced immunomodulation. This is in part governed by the actions of a network of cytokine interactions which, to date, remain largely undefined, and whose interspecific evolutionary conservation is unknown. This study applied Bayesian methods to illustrate the interrelationships between seminal profiles of interleukin (IL)-1alpha, IL-1beta, IL-2, IL-4, IL-5, IL-6, IL-9, IL-10, IL-12 (p70), IL-13, IL-17, eotaxin, granulocyte-colony stimulating factor (G-CSF), granulocyte macrophage-colony stimulating factor (GM-CSF), interferon (IFN)-gamma, keratinocyte-derived chemokine (KC), monocyte chemoattractant protein (MCP-1), macrophage inflammatory protein (MIP-1) alpha, MIP-1beta, regulated on activation normal T cell expressed and secreted (RANTES), tumour necrosis factor (TNF)-alpha, leptin, inducible protein (IP)-10 and vascular endothelial growth factor (VEGF) in a rat model. IL-2, IL-9, IL-12 (p70), IL-13, IL-18, eotaxin, IFN-gamma, IP-10, KC, leptin, MCP-1, MIP-1alpha and TNF-alpha were significantly higher in serum, whilst IL-1beta, IL-5, IL-6, IL-10, IL-17, G-CSF and GM-CSF were significantly higher in seminal fluid. When compared to mouse profiles, only G-CSF was present at significantly higher levels in the seminal fluid in both species. Bayesian modelling highlighted key shared features across mouse and rat networks, namely TNF-alpha as the terminal node in both serum and seminal plasma, and MCP-1 as a central coordinator of seminal cytokine networks through the intermediary of KC and RANTES. These findings reveal a marked interspecific conservation of seminal cytokine networks

Kepler Planet-Detection Mission: Introduction and First Results

The Kepler mission was designed to determine the frequency of Earth-sized planets in and near the habitable zone of Sun-like stars. The habitable zone is the region where planetary temperatures are suitable for water to exist on a planet’s surface. During the first 6 weeks of observations, Kepler monitored 156,000 stars, and five new exoplanets with sizes between 0.37 and 1.6 Jupiter radii and orbital periods from 3.2 to 4.9 days were discovered. The density of the Neptune-sized Kepler-4b is similar to that of Neptune and GJ 436b, even though the irradiation level is 800,000 times higher. Kepler-7b is one of the lowest-density planets (~0.17 gram per cubic centimeter) yet detected. Kepler-5b, -6b, and -8b confirm the existence of planets with densities lower than those predicted for gas giant planets

Characteristics of planetary candidates observed by Kepler. II. Analysis of the first four months of data

On 2011 February 1 the Kepler mission released data for 156,453 stars observed from the beginning of the science observations on 2009 May 2 through September 16. There are 1235 planetary candidates with transit-like signatures detected in this period. These are associated with 997 host stars. Distributions of the characteristics of the planetary candidates are separated into five class sizes: 68 candidates of approximately Earth-size (Rp &lt; 1.25 R⊕), 288 super-Earth-size (1.25 R⊕ ≤ R p &lt; 2 R⊕), 662 Neptune-size (2 R ⊕ ≤ Rp &lt; 6 R⊕), 165 Jupiter-size (6 R⊕ ≤ Rp &lt; 15 R ⊕), and 19 up to twice the size of Jupiter (15 R ⊕ ≤ Rp &lt; 22 R⊕). In the temperature range appropriate for the habitable zone, 54 candidates are found with sizes ranging from Earth-size to larger than that of Jupiter. Six are less than twice the size of the Earth. Over 74% of the planetary candidates are smaller than Neptune. The observed number versus size distribution of planetary candidates increases to a peak at two to three times the Earth-size and then declines inversely proportional to the area of the candidate. Our current best estimates of the intrinsic frequencies of planetary candidates, after correcting for geometric and sensitivity biases, are 5% for Earth-size candidates, 8% for super-Earth-size candidates, 18% for Neptune-size candidates, 2% for Jupiter-size candidates, and 0.1% for very large candidates; a total of 0.34 candidates per star. Multi-candidate, transiting systems are frequent; 17% of the host stars have multi-candidate systems, and 34% of all the candidates are part of multi-candidate systems