bluuebunny/crossref_metadata_2025_split huggingface dataset:
A cross-sectional assessment of food- and nutrient-based standards applied to British schoolchildren’s packed lunches
Authors: Evans Charlotte EL , Cade Janet E 
Published: September 2016

AbstractObjectiveIn England, standards for school meals included both foods and nutrients until 2015. School policies for packed lunches are generally food based; research is needed to determine whether these are adequate or whether a small number of nutrients would potentially improve their quality.DesignFrom dietary data obtained using a weighed dietary assessment tool, a diet quality score (DQS) for packed lunches was calculated using the number of standards met out of twenty-one (eight foods and thirteen nutrients). Multilevel regression analysis determined the foods and nutrients contributing to variation in the DQS.SettingEighty-nine primary schools across the four regions of the UK (England, Wales, Scotland and Northern Ireland).SubjectsBritish schoolchildren (n 1294), aged 8–9 years, taking a packed lunch.ResultsThe optimal model included all eight foods and seven of the thirteen nutrients, explaining 72 % of the variance in DQS. Folate, Fe and vitamin C, together with the eight food groups, explained 70 % of DQS variation.ConclusionsIdeally, policies for school packed lunches should include food-based standards plus recommendations based on a small number of nutrients.
Estimation of true height: a study in population-specific methods among young South African adults
Authors: Lahner Christen Renée , Kassier Susanna Maria , Veldman Frederick Johannes 
Published: September 2016

AbstractObjectiveTo investigate the accuracy of arm-associated height estimation methods in the calculation of true height compared with stretch stature in a sample of young South African adults.DesignA cross-sectional descriptive design was employed.SettingPietermaritzburg, Westville and Durban, KwaZulu-Natal, South Africa, 2015.SubjectsConvenience sample (N 900) aged 18–24 years, which included an equal number of participants from both genders (150 per gender) stratified across race (Caucasian, Black African and Indian).ResultsContinuous variables that were investigated included: (i) stretch stature; (ii) total armspan; (iii) half-armspan; (iv) half-armspan ×2; (v) demi-span; (vi) demi-span gender-specific equation; (vii) WHO equation; and (viii) WHO-adjusted equations; as well as categorization according to gender and race. Statistical analysis was conducted using IBM SPSS Statistics Version 21.0. Significant correlations were identified between gender and height estimation measurements, with males being anatomically larger than females (P<0·001). Significant differences were documented when study participants were stratified according to race and gender (P<0·001). Anatomical similarities were noted between Indians and Black Africans, whereas Caucasians were anatomically different from the other race groups. Arm-associated height estimation methods were able to estimate true height; however, each method was specific to each gender and race group.ConclusionsHeight can be calculated by using arm-associated measurements. Although universal equations for estimating true height exist, for the enhancement of accuracy, the use of equations that are race-, gender- and population-specific should be considered.
Descriptive figures for differences in parenting and infant night-time distress in the first three months of age
Authors: St James-Roberts Ian , Roberts Marion , Hovish Kimberly , Owen Charlie 
Published: September 2016

AimTo provide descriptive figures for infant distress and associated parenting at night in normal London home environments during the first three months of age.BackgroundMost western infants develop long night-time sleep periods by four months of age. However, 30% of infants in many countries sleep for short periods and cry out on waking in the night: the most common type of infant sleep behaviour problem. Preventive interventions may help families and improve services. There is evidence that ‘limit-setting’ parenting, which is common in western cultures, supports the development of settled infant night-time behaviour. However, a recent review has challenged this and argued that this form of parenting risks distressing infants. This study describes limit-setting parenting as practiced in London, compares it with ‘infant-cued’ parenting and measures the associated infant distress.MethodsLongitudinal infrared video, diary and questionnaire observations comparing a General-Community (n=101) group and subgroups with a Bed-Sharing (n=19) group on measures of infant and parenting behaviours at night.FindingsGeneral-Community parents took longer to detect and respond to infant waking and signalling, and to begin feeding, compared with the highly infant-cued care provided by Bed-Sharing parents. The average latency in General-Community parents’ responding to infant night-time waking was 3.5 min, during which infants fuss/cried for around 1 min. Compared with Bed-Sharing parenting, General-Community parenting was associated with increased infant distress of around 30 min/night at two weeks, reducing to 12 min/night by three months of age. However, differences in infant distress between General-Community subgroups adopting limit-setting versus infant-cued parenting were not large or statistically significant at any age. The figures provide descriptive evidence about limit-setting parenting which may counter some doubts about this form of parenting and help parents and professionals to make choices.
Anglicanism, Uhuru and Ujamaa: Anglicans in Tanzania and the Movement for Independence
Authors: Mndolwa Maimbo , Denis Philippe 
Published: September 2016

AbstractThe Anglican Church in Tanzania emerged from the work of the Universities’ Mission to Central Africa (UMCA) and the Australian Church Missionary Society (CMSA). The Anglican missions had goals which stood against colonialism and supported the victory of nationalism. Using archives and interviews as sources, this article considers the roles and reaction of the Anglican missions in the struggle for political independence in Tanganyika and Zanzibar, the effects of independence on the missions and the Church more broadly, and the responses of the missions to ujamaa in Tanzania.
Optical hydrogen absorption consistent with a bow shock around the hot Jupiter HD 189733 b
Authors: Cauley P. Wilson , Redfield Seth , Jensen Adam G. , Barman Travis , Endl Michael , Cochran William D. 
Published: September 2016

AbstractHot Jupiters, i.e., Jupiter-mass planets with orbital semi major axes of <10 stellar radii, can interact strongly with their host stars. If the planet is moving supersonically through the stellar wind, a bow shock will form ahead of the planet where the planetary magnetosphere slams into the the stellar wind or where the planetary outflow and stellar wind meet. Here we present high resolution spectra of the hydrogen Balmer lines for a single transit of the hot Jupiter HD 189733 b. Transmission spectra of the Balmer lines show strong absorption ~70 minutes before the predicted optical transit, implying a significant column density of excited hydrogen orbiting ahead of the planet. We show that a simple geometric bow shock model is able to reproduce the important features of the absorption time series while simultaneously matching the line profile morphology. Our model suggests a large planetary magnetic field strength of ~28 G. Follow-up observations are needed to confirm the pre-transit signal and investigate any variability in the measurement.
Ultraviolet and X-ray irradiance and flares from low-mass exoplanet host stars
Authors: France Kevin , Loyd R. O. Parke , Brown Alex 
Published: September 2016

AbstractThe spectral and temporal behavior of exoplanet host stars is a critical input to models of the chemistry and evolution of planetary atmospheres. High-energy photons (X-ray to NUV) from these stars regulate the atmospheric temperature profiles and photochemistry on orbiting planets, influencing the production of potential “biomarker” gases. We report first results from the MUSCLES Treasury Survey, a study of time-resolved UV and X-ray spectroscopy of nearby M and K dwarf exoplanet host stars. This program uses contemporaneous Hubble Space Telescope and Chandra (or XMM) observations to characterize the time variability of the energetic radiation field incident on the habitable zones planetary systems at d ≲ 20 pc. We find that all exoplanet host stars observed to date exhibit significant levels of chromospheric and transition region UV emission. M dwarf exoplanet host stars display 30–7000% UV emission line amplitude variations on timescales of minutes-to-hours. The relative flare/quiescent UV flux amplitudes on weakly active planet-hosting M dwarfs are comparable to active flare stars (e.g., AD Leo), despite their weak optical activity indices (e.g., Ca II H and K equivalent widths). We also detect similar UV flare behavior on a subset of our K dwarf exoplanet host stars. We conclude that strong flares and stochastic variability are common, even on “optically inactive” M dwarfs hosting planetary systems. These results argue that the traditional assumption of weak UV fields and low flare rates on older low-mass stars needs to be revised.
White-light continuum in stellar flares
Authors: Kowalski Adam F. 
Published: September 2016

AbstractIn this talk, we discuss the formation of the near-ultraviolet and optical continuum emission in M dwarf flares through the formation of a dense, heated chromospheric condensation. Results are used from a recent radiative-hydrodynamic model of the response of an M dwarf atmosphere to a high energy flux of nonthermal electrons. These models are used to infer the charge density and optical depth in continuum emitting flare layers from spectra covering the Balmer jump and optical wavelength regimes. Future modeling and observational directions are discussed.
Synthetic activity indicators for M-type dwarf stars
Authors: Wedemeyer Sven , Ludwig Hans-Günter 
Published: September 2016

AbstractHere, we present a set of time-dependent 3D RMHD simulations of a M-dwarf star representative of AD Leo, which extend from the upper convection zone into the chromosphere. The 3D model atmospheres are characterized by a very dynamic and intermittent structure on small spatial and temporal scales and a wealth of physical processes, which by nature cannot be described by means of 1D static model atmospheres. Artificial observations of these models imply that a combination of complementary diagnostics such as Ca II lines and the continuum intensity from UV to millimeter wavelengths, probe various properties of the dynamics, thermal and magnetic structure of the photosphere and the chromosphere and thus provide measures of stellar activity, which can be compared to observations. The complicated magnetic field structure and its imprint in synthetic diagnostics may have important implications for the understanding and characterization of stellar activity and with it possibly for the evaluation of planetary habitability around active M-dwarf stars.
CARMENES: M dwarfs and their planets
Authors: Quirrenbach A. , Amado P.J. , Caballero J.A. , Mandel H. , Mundt R. , Reiners A. , Ribas I. , Seifert W. , Azzaro M. , Galadí D. ,   the CARMENES Consortium
Published: September 2016

AbstractCARMENES (Calar Alto high-Resolution search for M dwarfs with Exo-earths with Near-infrared and optical Echelle Spectrographs) is a new instrument currently undergoing commissioning at the 3.5 m telescope of the Calar Alto Observatory. It has been constructed by a consortium of eleven Spanish and German institutions. The scientific goal of the project is a 600-night radial-velocity survey targeting 300 M dwarfs with sufficient precision to detect terrestrial planets in their habitable zones. The CARMENES instrument consists of two separate échelle spectrographs covering the wavelength range from 0.55 to 1.7 μm at a spectral resolution of R = 82,000, fed by fibers from the Cassegrain focus of the telescope. Both spectrographs are housed in a temperature-stabilized environment in vacuum tanks, to enable a long-term radial velocity precision of 1 m s−1. The wavelength calibration will be done with Th-Ne and U-Ne emission line lamps, and with Fabry-Pérot etalons.
Flares from ultracool L dwarfs with Kepler
Authors: Gizis John E. , Paudel Rishi , Williams Peter K. G. , Burgasser Adam J. , Schmidt Sarah J. 
Published: September 2016

AbstractWe report on our search for L dwarf flares using NASA's Kepler mission. Spectroscopically confirmedflares were detected with the original Kepler mission from an L1 dwarf stars. We discuss the physicalcharacteristics of these white light flares and compare them to M dwarf flares. For “habitable zone” planets, the apparent flare brightnesses would be comparable to the most powerful M dwarf flares. Weare monitoring more L dwarfs with the Kepler K2 mission. We discussthe prospect for more detections during the remainder of the K2 mission.
Fermi Large Area Telescope observation of high-energy solar flares: constraining emission scenarios
Authors: Omodei Nicola , Pesce-Rollins Melissa , Petrosian Vahè , Liu Wei , da Costa Fatima Rubio , Allafort Alice ,   for the Fermi-LAT collaboration
Published: September 2016

AbstractThe Fermi Large Area Telescope (LAT) is the most sensitive instrument ever deployed in space for observing gamma-ray emission >100 MeV. This has also been demonstrated by its detection of quiescent gamma-ray emission from pions produced by cosmic-ray protons interacting in the solar atmosphere, and from cosmic-ray electron interactions with solar optical photons. The Fermi-LAT has also detected high-energy gamma-ray emission associated with GOES M-class and X-class solar flares, each accompanied by a coronal mass ejection and a solar energetic particle event, increasing the number of detected solar flares by almost a factor of 10 with respect to previous space observations. During the impulsive phase, gamma rays with energies up to several hundreds of MeV have been recorded by the LAT. Emission up to GeV energies lasting several hours after the flare has also been detected by the LAT. Of particular interest are the recent detections of three solar flares whose position behind the limb was confirmed by the STEREO satellites. While gamma-ray emission up to tens of MeV resulting from proton interactions has been detected before from occulted solar flares, the significance of these particular events lies in the fact that these are the first detections of >100 MeV gamma-ray emission from footpoint-occulted flares. We will present the Fermi-LAT, RHESSI and STEREO observations of these flares and discuss the various emission scenarios for these sources.
Stellar flares and the dark energy of CMEs
Authors: Drake Jeremy J. , Cohen Ofer , Garraffo Cecilia , Kashyap V. 
Published: September 2016

AbstractFlares we observe on stars in white light, UV or soft X-rays are probably harbingers of coronal mass ejections (CMEs). If we use the Sun as a guide, large stellar flares will dissipate two orders of magnitude less X-ray radiative energy than the kinetic energy in the associated CME. Since coronal emission on active stars appears to be dominated by flare activity, CMEs pose a quandary for understanding the fraction of their energy budget stars can spend on magnetic activity. One answer is magnetic suppression of CMEs, in which the strong large-scale fields of active stars entrap and prevent CMEs unless their free energy exceeds a critical value. The CME-less flaring active region NOAA 2192 presents a possible solar analogue of this. Monster CMEs will still exist, and have the potential to ravage planetary atmospheres.
Solar flare soft X-ray spectra from Diogeness observations
Authors: Stȩślicki Marek , Sylwester Janusz , Sylwester Barbara , Szaforz Żaneta , Kordylewski Zbigniew , Płocieniak Stefan , Siarkowski Marek , Phillips Kenneth J. H. 
Published: September 2016

AbstractDiogeness was an uncollimated scanning flat crystal spectrometer observing solar flare X-ray spectra in four narrow wavelength bands in the vicinity of Ca xix, S xv and Si xiii He-like line ‘triplets’ around 3.18 Å, 5.04 Å and 6.65 Å. In two of the spectral channels, emission lines around the Ca xix 3.178 Å resonance line were scanned in opposite directions, being diffracted from precisely adjusted identical Quartz crystals mounted on a common shaft in a so-called Dopplerometer (tachometer) configuration. Observations of solar X-ray spectra made by Diogeness provide a direct diagnostic information on plasma characteristics during the impulsive flare energy release. We present a sample of events which occurred during the Diogeness operation time from August 16, 2001 to September 17, 2001.
Response of chromospheric lines to different periodic non-thermal electron beams
Authors: Cheng Jianxia , Ding Mingde 
Published: September 2016

AbstractSolar flares produce radiations in very broad wavelengths. Spectra can supply us abundant information about the local plasma, such as temperature, density, mass motion and so on. Strong chromospheric lines, like the most studied Hα and Ca II 8542 Å lines are formed under conditions of departures from local thermodynamic equilibrium in the lower atmosphere subject to flare heating. Understanding how these lines are formed is very useful for us to correctly interpret the observations. In this paper, we try to figure out the response of chromospheric lines heated by different periodic non-thermal electron beams. Our results are based on radiative hydrodynamic simulations. We vary the periods of electron beam injection from 1.25 s to 20 s. We compare the response times to different heating parameters. Possible explanations are discussed.
Solar extreme ultraviolet (EUV) flare observations and findings from the Solar Dynamics Observatory (SDO) EUV Variability Experiment (EVE)
Authors: Woods Thomas N. , Eparvier Francis G. , Mason James P. 
Published: September 2016

AbstractNew solar soft X-ray (SXR) and extreme ultraviolet (EUV) irradiance observations from NASA Solar Dynamics Observatory (SDO) EUV Variability Experiment (EVE) provide full coverage from 0.1 to 106 nm and continuously at a cadence of 10 seconds for spectra at 0.1 nm resolution. These observations during flares can usually be decomposed into four distinct characteristics: impulsive phase, gradual phase, coronal dimming, and EUV late phase. Over 6000 flares have been observed during the SDO mission; some flares show all four phases, and some only show the gradual phase. The focus is on the newer results about the EUV late phase and coronal dimming and its relationship to coronal mass ejections (CMEs). These EVE flare measurements are based on observing the sun-as-a-star, so these results could exemplify stellar flares. Of particular interest is that new coronal dimming measurements of stars could be used to estimate mass and velocity of stellar CMEs.
Observations and modeling of the ultraviolet emission of solar flares
Authors: Mikuła Katarzyna , Berlicki Arkadiusz , Heinzel Petr 
Published: September 2016

AbstractIn this paper we present the method of using far UV spectra of the flare observed by Interface Region Imaging Spectrograph (IRIS) for determination of the contribution of the continuum emission to the total UV radiation observed e.g. by SDO in 1600 Å channel. In our method the Si IV (1402.77 Å) line observed by IRIS is used as a proxy of C IV line emission contained in SDO/AIA UV images. Determined intensity of the flare continuum emission can be used to study the physics of the flare heated chromosphere and for better understanding of the emission mechanisms.
Discovery of superflares
Authors: Nogami Daisaku 
Published: September 2016

AbstractWe have discovered 1547 ‘superflares’ on about 279 G-type main-sequence stars by using the Kepler-spacecraft data of Q0-Q6. ‘Superflares’ mean flares that radiate total energy 10 times or more larger than that of the largest flare in the Sun ever recorded. We here briefly review our current understandings on superflares and superflare stars obtained by analyzing the Kepler data and follow-up high dispersion spectra.
Characterization of X-ray flare properties of AB Dor
Authors: Lalitha S. 
Published: September 2016

AbstractThe strong similarities between the flares observed on the Sun and in low mass stars has raised question regarding dynamo in these stars. Using the Sun as a prototype, one may be able to address this. In this paper, we present an analysis of 30 intense X-ray flares observed from AB Dor. These flares detected in XMM-Newton data show a rapid rise (500-3000 s) and a slow decay (1000-6000 s). Our studies suggest that the scaling law between the flare peak emission measure and the flare peak temperature for all the flares observed on AB Dor is very similar to the relationship followed by solar flares. Furthermore, we obtain the frequency distribution of flare energies which is a crucial diagnostic to calculate the overall energy residing in a flare. Our results of this study indicate that the large flare (1033 ≤ E ≤ 1034 erg) may not contribute to the heating of the corona.
White-light continuum emission from a solar flare and plage
Authors: Berlicki Arkadiusz , Awasthi Arun Kumar , Heinzel Petr , Sobotka Michal 
Published: September 2016

AbstractObservations of flare emissions in the optical continuum are very rare. Therefore, the analysis of such observations is useful and may contribute to our understanding of the flaring chromosphere and photosphere. We study the white light continuum emission observed during the X6.9 flare. This emission comes not only from the flare ribbons but also form the nearby plage area. The main aim of this work is to disentangle the flare and plage (facula) emission. We analyzed the spatial, spectral and temporal evolution of the flare and plage properties by analyzing multi-wavelength observations. We study the morphological correlation of the white-light continuum emission observed with different instruments. We found that some active region areas which produce the continuum emission correspond rather to plages than to the flare kernels. We showed that in some cases the continuum emission from the WL flare kernels is very similar to the continuum emission of faculae.
The frequency of stellar X-ray flares from a large-scale XMM-Newton sample
Authors: Pye John P. , Rosen Simon R. 
Published: September 2016

AbstractWe present estimates of cool-star X-ray flare rates determined from the XMM-Tycho survey (Pyeet al. 2015, A&A, 581, A28), and compare them with previously published values for the Sun and for other stellar EUV and white-light samples. We demonstrate the importance of applying appropriate corrections, especially in regard to the total, effective size of the stellar sample. Our results are broadly consistent with rates reported in the literature for Kepler white-light flares from solar-type stars, and with extrapolations of solar flare rates, indicating the potential of stellar X-ray flare observations to address issues such as ‘space weather’ in exoplanetary systems and our own solar system.