We report the discovery of two new transiting hot Jupiters, KOI-135b and KOI-204b, which were previously identified as planetary candidates by the Kepler team, and independently confirm the planetary ...nature of Kepler-17b, recently announced by Desert et al. (2011, ApJS, 197, 14). Radial-velocity measurements, taken with the SOPHIE spectrograph at the Observatoire de Haute-Provence (France), and Kepler photometry (Q1 and Q2 data) were used to derive the orbital, stellar, and planetary parameters. KOI-135b and KOI-204b orbit their parent stars in similar to 3.02 and 3.25 days, respectively. They have approximately the same radius, R-p = 1.20 +/- 0.06 R-Jup and 1.24 +/- 0.07 R-Jup, but different masses M-p = 3.23 +/- 0.19 M-Jup and 1.02 +/- 0.07 M-Jup. As a consequence, their bulk densities differ by a factor of four, rho(p) = 2.33 +/- 0.36 g cm(-3) (KOI-135b) and 0.65 +/- 0.12 g cm(-3) (KOI-204b), meaning that their interior structures are different. All three planets orbit metal-rich stars with Fe/H similar to 0.3 dex. Our SOPHIE spectra of Kepler-17 were used both to measure the radial-velocity variations and to determine the stellar atmospheric parameters, allowing us to refine the characterisation of the planetary system. In particular we found the radial-velocity semi-amplitude and the stellar mass to be respectively slightly smaller and larger than in Desert et al. These two quantities, however, compensate and lead to a fully consistent planetary mass. Our analysis gives M-p = 2.47 +/- 0.10 M-Jup and R-p = 1.33 +/- 0.04 R-Jup. We found evidence of a younger age for this planetary system, t \textless 1.8 Gyr, which is supported by both evolutionary tracks and gyrochronology. Finally, we confirm the detection of the optical secondary eclipse by Desert et al. and also find the brightness phase variation with the Q1 and Q2 Kepler data. The latter indicates a low redistribution of stellar heat to the night side (\textless16% at 1-sigma), if the optical planetary occultation comes entirely from thermal flux. The geometric albedo is A(g) \textless 0.12 (1-sigma).
In this paper, we present our HARPS radial-velocity data for eight low-activity solar-type stars belonging to the HARPS volume-limited sample: HD6718, HD8535, HD28254, HD290327, HD43197, HD44219, ...HD148156, and HD156411. Keplerian fits to these data reveal the presence of low-mass companions around these targets. With minimum masses ranging from 0.58 to 2.54 MJup, these companions are in the planetary mass domain. The orbital periods of these planets range from slightly less than one to almost seven years. The eight orbits presented in this paper exhibit a wide variety of eccentricities: from 0.08 to above 0.8.
In this paper we present a study of chemical abundances in six star- forming regions. Stellar parameters and metallicities are derived using high- resolution, high S/N spectra of weak-line T-Tauri ...stars in each region. The results show that nearby star-forming regions have a very small abundance dispersion (only 0.033 dex in Fe/H). The average metallicity found is slightly below that of the Sun, although compatible with solar once the errors are taken into account. The derived abundances for Si and Ni show that the observed stars have the abundances typical of Galactic thin disk stars of the same metallicity. The impact of these observations is briefly discussed in the context of the Galactic chemical evolution, local inter-stellar medium abundances, and in the origin of metal-rich stars in the solar neighbourhood (namely, stars more likely to harbour planets). The implication for future planet-search programmes around very young, nearby stars is also discussed.
Nucleotide sequences of two regions of the genomes of 11 yellow fever virus (YFV) samples isolated from monkeys or humans with symptomatic yellow fever (YF) in Brazil in 2000, 2004, and 2008 were ...determined with the objective of establishing the genotypes and studying the genetic variation. Results of the Bayesian phylogenetic analysis showed that sequences generated from strains from 2004 and 2008 formed a new subclade within the clade 1 of the South American genotype I. The new subgroup is here designated as 1E. Sequences of YFV strains recovered in 2000 belong to the subclade 1D, which comprises previously characterized YFV strains from Brazil. Molecular dating analyses suggested that the new subclade 1E started diversifying from 1D about 1975 and that the most recent 2004-2008 isolates arose about 1985. J. Med. Virol. 82:175-185, 2010.
We present new Ultraviolet and Visual Echelle Spectrograph (UVES) spectra of a sample of 15 cool unevolved stars with and without detected planetary companions. Together with previous determinations, ...we study Be depletion and possible differences in Be abundances between the two groups of stars. We obtain a final sample of 89 and 40 stars with and without planets, respectively, which covers a wide range of effective temperatures, from 4700 K to 6400 K, and includes several cool dwarf stars for the first time. We determine Be abundances for these stars and find that for most of them (the coolest ones) the Be II resonance lines are often undetectable, implying significant Be depletion. While for hot stars Be abundances are approximately constant, with a slight fall as T sub(eff) decreases and the Li-Be gap around 6300 K, we find a steep drop of Be content as T sub(eff) decreases for T sub(eff) < 5500 K, confirming the results of previous papers. Therefore, for these stars there is an unknown mechanism destroying Be that is not reflected in current models of Be depletion. Moreover, this strong Be depletion in cool objects takes place for all the stars regardless of the presence of planets; thus, the effect of extra Li depletion in solar-type stars with planets when compared with stars without detected planets does not seem to be present for Be, although the number of stars at those temperatures is still small to reach a final conclusion.
Purpose: This study aims to assess self-care in patients with non-optimal diabetes management (HbAlc >7.0% for adults and >8.0 for those aged 60 or over) and the positive and negative experiences ...associated with it in the rural communities of a Brazilian municipality. Patient and Methods: This is a cross-sectional mixed-methods study. The data were collected from participants with high HbA1c through focus group discussions, subsequently performing thematic analysis, and through structured questionnaires (socioeconomic characteristics and the Summary of Diabetes Self-Care Activities (SDSCA)). Results: The mean HbAlc of the 156 study participants was 9.94% (95% confidence interval: 9.70-10.19%) and most participants (86.54%) had negative self-care behaviors, with an overall SDSCA mean score of 3.55. This mean was not positive for any of the socioeconomic characteristics. The self-care activities with the most satisfactory performance concerned non-smoking and the use of prescribed medications, and the poorest results were observed for the practice of specific physical activities. The qualitative data indicated that the study participants face many difficulties regarding self-care practices, especially those related to an adequate diet. Conclusion: The self-care assessment revealed unsatisfactory self-care behaviors as well as high HbA1c levels among the study participants and highlighted the various difficulties they encounter. This indicates the need for more attentive health teams to monitor patients, especially regarding actions focused on the non-pharmacological elements of self-care, such as lifestyle changes, which were found to be the dimensions with the most unsatisfactory results. Keywords: primary care, non-communicable diseases, behaviors, rural communities
We report the discovery of a new planet candidate orbiting the subgiant star HD 118203 with a period of P -- 6.1335 days. The best Keplerian solution yields an eccentricity e = 0.31 and a minimum ...mass m2 sin i = 2.1 MJup for the planet. This star has been observed with the ELODIE fiber-fed spectrograph as one of the targets in our planet-search programme biased toward high-metallicity stars, on-going since March 2004 at the Haute-Provence Observatory. An analysis of the spectroscopic line profiles using line bisectors revealed no correlation between the radial velocities and the line-bisector orientations, indicating that the periodic radial-velocity signal is best explained by the presence of a planet-mass companion. A linear trend is observed in the residuals around the orbital solution that could be explained by the presence of a second companion in a longer-period orbit. We also present here our orbital solution for another slightly evolved star in our metal-rich sample, HD 149143, recently proposed to host a 4-d period Hot Jupiter by the N2K consortium. Our solution yields a period P - 4.09 days, a marginally significant eccentricity e -- 0.08 and a planetary minimum mass of 1.36 MJup. We checked that the shape of the spectral lines does not vary for this star as well.
A combined heart rate (HR) and motion sensor (Actiheart) has been proposed as an accurate method for assessing total energy expenditure (TEE) and physical activity energy expenditure (PAEE). However, ...the extent to which factors such as caffeine may affect the accuracy by which the estimated HR-related PAEE contribution will affect TEE and PAEE estimates is unknown. Therefore, we examined the validity of Actiheart in estimating TEE and PAEE in free-living adults under a caffeine trial compared with doubly labeled water (DLW) as reference criterion.
Using a double-blind crossover trial (Clinicaltrials.gov ID: #NCT01477294) with two conditions (4-day each with a 3-day-washout period), randomly ordered as caffeine (5 mg/kg per day) and placebo (malt-dextrine) intake, TEE was measured by DLW in 17 physically active men (20-38 years) who were non-caffeine users. In each condition, resting energy expenditure (REE) was assessed by indirect calorimetry and PAEE was calculated as (TEE-(REE+0.1 TEE)). Simultaneously, PAEE and TEE were estimated by Actiheart using an individual calibration (ACC+HRstep).
Under caffeine, ACC+HRstep explained 76 and 64% of TEE and PAEE from DLW, respectively; corresponding results for the placebo condition were 82 and 66%. No mean bias was found between ACC+HRstep and DLW for TEE (caffeine:-468 kJ per day; placebo:-407 kJ per day), although PAEE was slightly underestimated (caffeine:-856 kJ per day; placebo:-1147 kJ per day). Similar limits of agreement were observed in both conditions ranging from -2066 to 3002 and from -3488 to 1776 kJ per day for TEE and PAEE, respectively.
Regardless of caffeine intake, the combined HR and motion sensor is valid for estimating free-living energy expenditure in a group of healthy men but is less accurate for an individual assessment.
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