Práticas alimentares de crianças desnutridas menores de dois anos de idade

Analisar práticas alimentares de crianças desnutridas menores de dois anos. Estudo exploratório e descritivo, com análise qualitativa dos dados, realizado a partir de observação participante e entrevistas. Participaram 42 sujeitos. Os dados foram submetidos à análise temática. Ao explorar as práticas alimentares dessas crianças, os temas que emergiram foram: quem prepara a alimentação e o que é preparado; como são preparados os alimentos; a rotina alimentar das crianças; onde e como as crianças são servidas. A alimentação era pouco variada; láctea, no café da manhã e lanches, e no almoço com alimentos como arroz, batata, feijão e, às vezes, carnes. Frutas e hortaliças eram escassas, e alimentos industrializados estavam presentes em todos os domicílios. Foi possível apreender o cotidiano das práticas alimentares, suas inadequações, insuficiência de alimentos, higiene precária dos alimentos complementares, influência das avós, ambiente inadequado às refeições e situação de vida das famílias.

Acompanhamento do aleitamento materno no tratamento de crianças com fenilcetonúria

A fenilcetonúria (PKU) ocorre na incapacidade para transformar fenilalanina em tirosina, trazendo efeitos tóxicos para o sistema nervoso central. Tradicionalmente, no tratamento da PKU, o aleitamento materno é substituído por fórmula láctea. Este estudo verificou os efeitos do aleitamento materno como fonte de fenilalanina no desenvolvimento de crianças com PKU. Participaram dez lactentes com PKU, que iniciaram o tratamento com a introdução de fórmula láctea antes dos 30 dias e que mantiveram o aleitamento materno por no mínimo 30 dias de vida após o início dos procedimentos. Os procedimentos basearam-se em estimar a ingestão de leite materno, com margem segura da concentração da fenilalanina, calculando o volume gástrico e oferecendo inicialmente fórmula láctea, seguida do aleitamento materno em demanda livre, em todas as mamadas. O tempo de amamentação variou de um mês e cinco dias a 14 meses. Os controles sanguíneos foram semanais. Se o nível sérico da fenilalanina estivesse >2 mg/dL e <6 mg/dL mantinha-se a prescrição; se estivesse <2 mg/dL, diminuía-se a fórmula láctea em 25%, aumentando indiretamente o aleitamento materno; se estivesse >6 mg/dL, aumentava-se a fórmula em 50%. Avaliou-se os níveis de fenilalanina, aplicou-se a Early Language Milestone Scale e Passos Básicos do Desenvolvimento. Foram considerados adequados aqueles lactentes que apresentaram índices normativos em todas as avaliações. Dos lactentes, 80% conseguiram manter limites seguros da fenilalanina e desenvolvimento nos índices normativos. Há viabilidade da continuidade do aleitamento materno no tratamento de crianças com PKU desde que os níveis de fenilalanina sejam rigorosamente controlados e que os efeitos do aleitamento materno para o desenvolvimento infantil sejam verificados.

Segue 3: the youngest globular cluster in the outer halo

Deep Galileo (Telescopio Nazionale Galileo) B, V and I images of Segue 3, reaching V ∼ 25, reveal that it is the youngest globular cluster known so far in the Galaxy. A young age of 3.2 Gyr is found, differently from a previous estimate of 12 Gyr. It also appears to be moderately metal rich with [Fe/H] ∼ −0.8, rather than [Fe/H] ∼ −1.7, as previously suggested by Fadely et al. A main difference in the age derivation relative to Fadely et al. comes from the consideration of subgiant branch stars in the isochrone fitting. A deduced distance of d⊙ = 29.1 kpc is compatible with the outer halo location of other low luminosity globular clusters.

The star formation rate in the inner Milky Way Galaxy

The present star formation rate (SFR) in the inner Galaxy is puzzling for the chemical evolution models (CEM). No static CEM is able to reproduce the peak of the SFR in the 4 kpc ring. The main reason is probably a shortage of gas, which could be due to the dynamical effects produced by the galactic bar, not considered by these models. We developed a CEM that includes radial gas flows in order to mimic the effects of the galactic bar in the first 5 kpc of the galactic disk. In this model, the star formation (SF) is a two-step process: first, the diffuse gas forms molecular clouds. Then, stars form from cloud-cloud collisions or by the interaction between massive stars and the molecular gas. The former is called spontaneous and the latter induced SF. The mass in the different phases of each region changes by the processes associated with the stellar formation and death by: the SF due to spontaneous fragmentation of gas in the halo; formation of gas clouds in the disk from the diffuse gas; induced SF in the disk due to the interaction between massive stars and gas clouds; and finally, the restitution of the diffuse gas associated to these process of cloud and star formation. In the halo, the star formation rate for the diffuse gas follows a Schmidt law with a power n = 1.5. In the disk, the stars form in two steps: first, molecular clouds are formed from the diffuse gas also following a Schmidt law with n=1.5 and a proportionality factor. Including a specific pattern of radial gas flows, the CEM is able to reproduce with success the peak in the SFR at 4 kpc (fig. 1).

A galaxy model from Two Micron All Sky Survey star counts in the whole sky, including the plane

We use the star count model of Ortiz & Lépine to perform an unprecedented exploration of the most important Galactic parameters comparing the predicted counts with the Two Micron All Sky Survey observed star counts in the J, H, and KS bands for a grid of positions covering the whole sky. The comparison is made using a grid of lines of sight given by the HEALPix pixelization scheme. The resulting best-fit values for the parameters are: 2120 ± 200 pc for the radial scale length and 205 ± 40 pc for the scale height of the thin disk, with a central hole of 2070$_{-800}^{+2000}$ pc for the same disk, 3050 ± 500 pc for the radial scale length and 640 ± 70 pc for the scale height of the thick disk, 400 ± 100 pc for the central dimension of the spheroid, 0.0082 ± 0.0030 for the spheroid to disk density ratio, and 0.57 ± 0.05 for the oblate spheroid parameter.

Mass extinctions, galactic orbits in the solar neighborhood and the Sun: a connection?

The orbits of the stars in the disk of the Galaxy, and their passages through the Galactic spiral arms, are a rarely mentioned factor of biosphere stability which might be important for long-term planetary climate evolution, with a possible bearing on mass extinctions. The Sun lies very near the co-rotation radius, where stars revolve around the Galaxy in the same period as the density wave perturbations of the spiral arms. conventional wisdom generally considers that this status makes for few passages through the spiral arms. Controversy still surrounds whether time spent inside or around spiral arms is dangerous to biospheres and conductive to mass extinctions. Possible threats include giant molecular clouds disturbing the Oort comet cloud and provoking heavy bombardment: a higher exposure to cosmic rays near star forming regions triggering increased cloudiness in Earth atmosphere and ice ages; and the desctruction of Earth's ozone layer posed by supernova explosiosn. We present detailed calculations of the history of spiral arm passages for all 212 solar-type stars nearer than 20 parsecs, including the total time spent inside armsin the last 500 Myr, when the spiral arm position can be traced with good accuracy. We found that there is a large diversity of stellar orbits in the solar neighborhood, and the time fraction spent inside spiral arms can vary from a few percent to nearly half the time. The Sun, despite its proximity to the galactic co-rotation radius, has exceptionally low eccentricity and a low vertical velocity component, and therefore spends 30% of its lifetime crossing the spiral arms, more than most nearby stars. We discuss the possible implications of this fact to the long-term habitability of the Earth, and possible correlations of the Sun's passage through the spiral arms with the five great mass extinctions of the Earth's biosphere from the Late Ordovician to the Cretaceous-Tertiary.

A galaxy model from Two Micron All Sky Survey star counts in the whole sky, including the plane

We use the star count model of Ortiz & L´epine to perform an unprecedented exploration of the most important Galactic parameters comparing the predicted counts with the Two Micron All Sky Survey observed star counts in the J, H, and KS bands for a grid of positions covering the whole sky. The comparison is made using a grid of lines of sight given by the HEALPix pixelization scheme. The resulting best-fit values for the parameters are: 2120 ± 200 pc for the radial scale length and 205 ± 40 pc for the scale height of the thin disk, with a central hole of 2070+2000 −800 pc for the same disk, 3050 ± 500 pc for the radial scale length and 640 ± 70 pc for the scale height of the thick disk, 400 ± 100 pc for the central dimension of the spheroid, 0.0082 ± 0.0030 for the spheroid to disk density ratio, and 0.57 ± 0.05 for the oblate spheroid parameter.