bluuebunny/crossref_metadata_2025_split huggingface dataset:
Contrasting Nitrogen Fate in Watersheds Using Agricultural and Water Quality Information
Authors: Essaid Hedeff I. , Baker Nancy T. , McCarthy Kathleen A. 
Published: July 2016

Surplus nitrogen (N) estimates, principal component analysis (PCA), and end‐member mixing analysis (EMMA) were used in a multisite comparison contrasting the fate of N in diverse agricultural watersheds. We applied PCA‐EMMA in 10 watersheds located in Indiana, Iowa, Maryland, Nebraska, Mississippi, and Washington ranging in size from 5 to 1254 km2with four nested watersheds. Watershed Surplus N was determined by subtracting estimates of crop uptake and volatilization from estimates of N input from atmospheric deposition, plant fixation, fertilizer, and manure for the period from 1987 to 2004. Watershed average Surplus N ranged from 11 to 52 kg N ha−1and from 9 to 32% of N input. Solute concentrations in streams, overland runoff, tile drainage, groundwater (GW), streambeds, and the unsaturated zone were used in the PCA‐EMMA procedure to identify independent components contributing to observed stream concentration variability and the end‐members contributing to streamflow and NO3load. End‐members included dilute runoff, agricultural runoff, benthic‐processing, tile drainage, and oxic and anoxic GW. Surplus N was larger in watersheds with more permeable soils (Washington, Nebraska, and Maryland) that allowed greater infiltration, and oxic GW was the primary source of NO3load. Subsurface transport of NO3in these watersheds resulted in some removal of Surplus N by denitrification. In less permeable watersheds (Iowa, Indiana, and Mississippi), NO3was rapidly transported to the stream by tile drainage and runoff with little removal. Evidence of streambed removal of NO3by benthic diatoms was observed in the larger watersheds.Core IdeasStream NO3discharge trends reflect contributions from different NO3sources.Watersheds with more permeable soils had greater Surplus N.More permeable watersheds experienced greater N removal by denitrification.Less permeable watersheds transported surplus N directly to the stream.N removal by benthic processing was discerned in larger watersheds.
Comparison of Nutrient and Metal Loadings with the Application of Swine Manure Slurries and Their Liquid Separates to Soils
Authors: Kumaragamage D. , Akinremi O. O. , Racz G. J. 
Published: July 2016

The accumulation of phosphorus (P) and metals is a serious concern with the continuous application of manure to agricultural soils. Solid–liquid separation of swine slurry is a promising approach to reduce P and metal loadings through application of separated liquid (SL) as a nutrient source. However, little information is available on nutrient and metal loadings with the application of SL compared with unseparated raw manure (RM). We analyzed element concentrations and calculated nutrient and metal loadings for RM and their respective SL applications, considering an application rate of 100 kg total nitrogen (N) ha−1. Samples of SL were obtained through three separation techniques: (i) centrifugation without a flocculant, (ii) centrifugation with a flocculant, and (iii) rotary press with a flocculant. Irrespective of separation technique, calculated P loadings with the application of SL were only 50 to 70% of that of RM at equivalent rates of total N yet exceeded crop removal rate. In contrast, calculated K and Na loadings with SL application were significantly greater than with RM, indicating a possible build‐up of K and Na in soil. Calculated Ca and Mg loadings were significantly greater with RM than with SL. Loadings of Al, As, Ba, Cd, Cr, Fe, Mn, Ni, Pb, Sn, Se, Ti, and V were low, whereas Cu and Zn loadings were above crop removal rates for RM and SL. For solid–liquid separation to provide a lasting solution to the problem of P and metal accumulation, the SL must be supplemented with commercial N fertilizer to meet crop N demand.Core Ideas
P loading with SL was only 50 to 70% of that of swine slurry applied at equivalent rate of N.
Loadings of K and Na with SL were higher, indicating a possible salt build‐up in soil.
Cu and Zn loading with application of swine slurry and SL were above crop removal rates.
Loadings of other trace metals were low with both SL and raw swine slurry application.
Conselho de Políticas e Participação: Aspectos do Funcionamento do Conselho Municipal de Saúde de Belo Horizonte - MG
Authors: Lopes Bruno De Jesus , Silva Edson Arlindo , Martins Simone 
Published: July 2016

<p>Os Conselhos de Saúde (CS) foram reconhecidos no Brasil como espaços para interação da sociedade com o Estado nas decisões políticas sobre o Sistema Único de Saúde. A construção deste espaço pode ser compreendida como uma conquista da sociedade representando um contrapeso às formas de decisão centradas no governo. Com a institucionalização do conselho, começa a existir a possibilidade de inserção da sociedade nas discussões em torno de políticas públicas. Partindo deste contexto esta pesquisa teve como objetivo central conhecer o funcionamento do Conselho Municipal de Saúde de Belo Horizonte com base nas atas das plenárias do conselho, na Resolução 333 de 2003 e no Regimento Interno do conselho. O método de análise de dados utilizado para este trabalho foi análise documental, onde foi estudado as atas das plenárias do Conselho de 2004 a 2012 e a Análise de Conteúdo. Como resultado, pode ser destacado o adequado funcionamento do Conselho Municipal de Saúde de Belo Horizonte, no entanto, com baixo envolvimento dos representantes do Estado nos processos de tomadas de decisão o que pode prejudicar o alcance do objetivo do conselho que é a livre tomada de decisão pública.</p><p> </p>
Teorias da Ação Coletiva no Campo do Agronegócio: Uma Análise a Partir de Teses e Dissertações (1998-2012)
Authors: Wenningkamp Keila Raquel , Schmidt Carla Maria 
Published: July 2016

<p>A partir de 1990, diversas formas de ações coletivas passaram a ser encontradas no agronegócio, de maneira que essas vêm auxiliando consideravelmente para o desenvolvimento local e regional. Não apenas a presença de ações coletivas, mas também estudos sobre essa temática têm se tornado mais frequentes. Nesse sentido, o objetivo deste estudo foi o de analisar os resultados teórico-empíricos de teses e dissertações sobre ações coletivas no agronegócio, defendidas entre 1998 e 2012, à luz de teorias da ação coletiva. Ou seja, buscou-se comparar o que defendem teorias da ação coletiva, especialmente os enfoques de Olson, Granovetter e Ostrom, com os achados desses trabalhos científicos. Em termos metodológicos, este estudo apresenta abordagem qualitativa, de caráter descritivo. Como técnica de coleta de dados, utilizou-se a análise de conteúdo, a partir da leitura e interpretação dos objetivos e conclusões das teses e dissertações defendidas na temática, entre 1998 e 2012. Os principais resultados apontaram para a existência de uma série de benefícios proporcionados por meio da ação coletiva, tanto de cunho econômico como de social, ambiental e cultural. Dessa forma, a relação entre as teorias da ação coletiva e os achados teórico-empíricos das teses e dissertações conduz ao entendimento de que formas coletivas favorecem o desenvolvimento local e regional. Contudo, igualmente ficou latente a existência de diversos desafios, mas que, de modo geral, tendem a ser menores do que os benefícios gerados pelas ações coletivas. Concluiu-se que os resultados encontrados nas teses e dissertações puderam ser relacionados às teorias da ação coletiva.</p><p> </p>
Development of microsatellite markers for Crepis mollis (Asteraceae)
Authors: Duwe Virginia K. , Muller Ludo A. H. , Borsch Thomas , Ismail Sascha A. 
Published: July 2016

Premise of the study:Polymorphic microsatellite markers were developed for the threatened species Crepis mollis (Asteraceae) to investigate population and conservation genetics.Methods and Results:Illumina sequencing was conducted on pooled genomic DNA from 10 individuals of two populations. Ten polymorphic and 10 monomorphic microsatellite loci with di‐, tri‐, tetra‐, penta‐, and hexanucleotide repeat motifs were developed and characterized in C. mollis. In the polymorphic markers, up to 17 alleles per locus were detected with an observed and expected heterozygosity ranging from 0.120 to 0.780 and 0.102 to 0.834, respectively. Furthermore, the polymorphic markers were tested for cross‐amplification in three congeneric species (C. biennis, C. foetida, and C. sancta) and amplified in up to three loci.Conclusions:The markers developed in this study are the first microsatellites tested on C. mollis and will be useful for performing population and conservation genetic studies in this threatened species.
AVERAGE SPATIAL DISTRIBUTION OF COSMIC RAYS BEHIND THE INTERPLANETARY SHOCK—GLOBAL MUON DETECTOR NETWORK OBSERVATIONS
Authors: Kozai M. , Munakata K. , Kato C. , Kuwabara T. , Rockenbach M. , Lago A. Dal , Schuch N. J. , Braga C. R. , Mendonça R. R. S. , Jassar H. K. Al , Sharma M. M. , Duldig M. L. , Humble J. E. , Evenson P. , Sabbah I. , Tokumaru M. 
Published: July 2016

ABSTRACT
We analyze the galactic cosmic ray (GCR) density and its spatial gradient in Forbush Decreases (FDs) observed with the Global Muon Detector Network (GMDN) and neutron monitors (NMs). By superposing the GCR density and density gradient observed in FDs following 45 interplanetary shocks (IP-shocks), each associated with an identified eruption on the Sun, we infer the average spatial distribution of GCRs behind IP-shocks. We find two distinct modulations of GCR density in FDs, one in the magnetic sheath and the other in the coronal mass ejection (CME) behind the sheath. The density modulation in the sheath is dominant in the western flank of the shock, while the modulation in the CME ejecta stands out in the eastern flank. This east–west asymmetry is more prominent in GMDN data responding to ∼60 GV GCRs than in NM data responding to ∼10 GV GCRs, because of the softer rigidity spectrum of the modulation in the CME ejecta than in the sheath. The geocentric solar ecliptic-y component of the density gradient, G

y
, shows a negative (positive) enhancement in FDs caused by the eastern (western) eruptions, while G

z
shows a negative (positive) enhancement in FDs caused by the northern (southern) eruptions. This implies that the GCR density minimum is located behind the central flank of IP-shocks and propagating radially outward from the location of the solar eruption. We also confirmed that the average G

z
changes its sign above and below the heliospheric current sheet, in accord with the prediction of the drift model for the large-scale GCR transport in the heliosphere.
POWER BEAMING LEAKAGE RADIATION AS A SETI OBSERVABLE
Authors: Benford James N. , Benford Dominic J. 
Published: July 2016

ABSTRACT
The most observable leakage radiation from an advanced civilization may well be from the use of power beaming to transfer energy and accelerate spacecraft. Applications suggested for power beaming involve launching spacecraft to orbit, raising satellites to a higher orbit, and interplanetary concepts involving space-to-space transfers of cargo or passengers. We also quantify beam-driven launch to the outer solar system, interstellar precursors, and ultimately starships. We estimate the principal observable parameters of power beaming leakage. Extraterrestrial civilizations would know their power beams could be observed, and so could put a message on the power beam and broadcast it for our receipt at little additional energy or cost. By observing leakage from power beams we may find a message embedded on the beam. Recent observations of the anomalous star KIC 8462852 by the Allen Telescope Array (ATA) set some limits on extraterrestrial power beaming in that system. We show that most power beaming applications commensurate with those suggested for our solar system would be detectable if using the frequency range monitored by the ATA, and so the lack of detection is a meaningful, if modest, constraint on extraterrestrial power beaming in that system. Until more extensive observations are made, the limited observation time and frequency coverage are not sufficiently broad in frequency and duration to produce firm conclusions. Such beams would be visible over large interstellar distances. This implies a new approach to the SETI search: instead of focusing on narrowband beacon transmissions generated by another civilization, look for more powerful beams with much wider bandwidth. This requires a new approach for their discovery by telescopes on Earth. Further studies of power beaming applications should be performed, potentially broadening the parameter space of the observable features that we have discussed here.
HARD X-RAY EMISSIONS FROM CASSIOPEIA A OBSERVED BY INTEGRAL
Authors: Wang Wei , Li Zhuo 
Published: July 2016

ABSTRACT
Cassiopeia A (Cas A), as the nearby young remnant of a core-collapse supernova, is the best candidate for astrophysical studies in supernova explosion and its environment. We studied the hard X-ray emission from Cas A using the 10 year data of INTEGRAL observations, and first detected non-thermal continuum emission from the source up to 220 keV. The 44Ti line emission at 68 and 78 keV is confirmed by our observations with a mean flux of ∼(2.2 ± 0.4) × 10−5 ph cm−2 s−1, corresponding to a 44Ti yield in Cas A of (1.3 ± 0.4) × 10−4
M
⊙. The continuum emission from 3 to 500 keV can be fit with a thermal bremsstrahlung of kT ∼ 0.79 ± 0.08 keV plus a power-law model of Γ ∼ 3.13 ± 0.03. The non-thermal emission from Cas A is well fit by a power-law model without a cutoff up to 220 keV. This radiation characteristic is inconsistent with diffusive shock acceleration models with a remnant shock velocity of only 5000 km s−1. The central compact object in Cas A cannot significantly contribute to the emission above 80 keV. Some possible physical origins of the non-thermal emission above 80 keV from the remnant shock are discussed. We deduce that the asymmetrical supernova explosion scenario of Cas A is a promising scenario for the production of high-energy synchrotron radiation photons, where a portion of the ejecta with a velocity of ∼0.1c and opening angle of ∼10° can account for the 100 keV emission, as is consistent with the “jet” observed in Cas A.
STAR FORMATION ACTIVITY IN A YOUNG GALAXY CLUSTER AT Z = 0.866
Authors: Laganá T. F. , Ulmer M. P. , Martins L. P. , Cunha E. da 
Published: July 2016

ABSTRACT
The galaxy cluster RX J1257+4738 at z = 0.866 is one of the highest redshift clusters with a richness of multi-wavelength data, and is thus a good target to study the star formation–density relation at early epochs. Using a sample of spectroscopically confirmed cluster members, we derive the star-formation rates (SFRs) of our galaxies using two methods: (1) the relation between SFR and total infrared luminosity extrapolated from the observed Spitzer Multiband Imaging Photometer for Spitzer 24 μm imaging data; and (2) spectral energy distribution fitting using the MAGPHYS code, including eight different bands. We show that, for this cluster, the SFR–density relation is very weak and seems to be dominated by the two central galaxies and the SFR presents a mild dependence on stellar mass, with more massive galaxies having higher SFR. However, the specific SFR (SSFR) decreases with stellar mass, meaning that more massive galaxies are forming fewer stars per unit of mass, and thus suggesting that the increase in star-forming members is driven by cluster assembly and infall. If the environment is somehow driving the star formation, one would expect a relation between the SSFR and the cluster centric distance, but that is not the case. A possible scenario to explain this lack of correlation is the contamination by infalling galaxies in the inner part of the cluster, which may be on their initial pass through the cluster center. As these galaxies have higher SFRs for their stellar mass, they enhance the mean SSFR in the center of the cluster.
ON THE FOURIER AND WAVELET ANALYSIS OF CORONAL TIME SERIES
Authors: Auchère F. , Froment C. , Bocchialini K. , Buchlin E. , Solomon J. 
Published: July 2016

ABSTRACT
Using Fourier and wavelet analysis, we critically re-assess the significance of our detection of periodic pulsations in coronal loops. We show that the proper identification of the frequency dependence and statistical properties of the different components of the power spectra provides a strong argument against the common practice of data detrending, which tends to produce spurious detections around the cut-off frequency of the filter. In addition, the white and red noise models built into the widely used wavelet code of Torrence & Compo cannot, in most cases, adequately represent the power spectra of coronal time series, thus also possibly causing false positives. Both effects suggest that several reports of periodic phenomena should be re-examined. The Torrence & Compo code nonetheless effectively computes rigorous confidence levels if provided with pertinent models of mean power spectra, and we describe the appropriate manner in which to call its core routines. We recall the meaning of the default confidence levels output from the code, and we propose new Monte-Carlo-derived levels that take into account the total number of degrees of freedom in the wavelet spectra. These improvements allow us to confirm that the power peaks that we detected have a very low probability of being caused by noise.
THE FIRST DISCOVERY OF PRESOLAR GRAPHITE GRAINS FROM THE HIGHLY REDUCING QINGZHEN (EH3) METEORITE
Authors: Xu Yuchen , Lin Yangting , Zhang Jianchao , Hao Jialong 
Published: July 2016

ABSTRACT
Presolar graphite grains have been extensively studied, but are limited in carbonaceous chondrites, particularly in Murchison (CM2) and Orgueil (CI1), which sampled materials from the oxidizing regions in the solar nebula. Here, we report the first discovery of presolar graphite grains from the Qingzhen (EH3) enstatite chondrite which formed under a highly reducing condition. Eighteen presolar graphite grains were identified by C-isotope mapping of the low-density fraction (1.75–1.85 g cm−3) from Qingzhen acid residue. Another 58 graphite spherules were found in different areas of the same sample mount using a scanning electron microscope and were classified into three morphologies, including cauliflower, onion, and cauliflower–onion. The Raman spectra of these spherules vary from ordered, disordered, and glassy to kerogen-like, suggestive of a wide range of thermal metamorphisms. NanoSIMS analysis of the C- and Si-isotopes of these graphite spherules confirmed 23 presolar grains. The other 35 graphite spherules have no significant isotopic anomalies, but they share similar morphologies and Raman spectra with the presolar ones. Another three grains were identified during NanoSIMS analysis. Of all the 44 presolar graphite grains identified, six grains show 28Si-excesses, suggestive of supernovae origins, and four grains are 12C- and 29,30Si-rich, consistent with low-metallicity asymptotic giant branch star origins. Another two graphite spherules have extremely low 12C/13C ratios with marginal solar Si-isotopes. The morphologies, Raman spectra, and C- and Si-isotopic distributions of the presolar graphite grains from the Qingzhen enstatite chondrite are similar to those of the low-density fractions from Murchison carbonaceous chondrites. This study suggests a homogeneous distribution of presolar graphite grains in the solar nebula.
THE FIRST NEPTUNE ANALOG OR SUPER-EARTH WITH A NEPTUNE-LIKE ORBIT: MOA-2013-BLG-605LB
Authors: Sumi T. , Udalski A. , Bennett D. P. , Gould A. , Poleski R. , Bond I. A. , Skowron J. , Rattenbury N. , Pogge R. W. , Bensby T. , Beaulieu J. P. , Marquette J. B. , Batista V. , Brillant S. , Abe F. , Asakura Y. , Bhattacharya A. , Donachie M. , Freeman M. , Fukui A. , Hirao Y. , Itow Y. , Koshimoto N. , Li M. C. A. , Ling C. H. , Masuda K. , Matsubara Y. , Muraki Y. , Nagakane M. , Ohnishi K. , Oyokawa H. , Saito To. , Sharan A. , Sullivan D. J. , Suzuki D. , Tristram P. J. , Yonehara A. ,   (The MOA Collaboration), Szymański M. K. , Ulaczyk K. , Kozłowski S. , Wyrzykowski Ł. , Kubiak M. , Pietrukowicz P. , Pietrzyński G. , Soszyński I. ,   (The OGLE Collaboration), Han C. , Jung Y.-K. , Shin I.-G , Lee C-U. 
Published: July 2016

ABSTRACT
We present the discovery of the first Neptune analog exoplanet or super-Earth with a Neptune-like orbit, MOA-2013-BLG-605Lb. This planet has a mass similar to that of Neptune or a super-Earth and it orbits at 9 ∼ 14 times the expected position of the snow line, a
snow, which is similar to Neptune's separation of 11 a
snow from the Sun. The planet/host-star mass ratio is q = (3.6 ± 0.7) × 10−4 and the projected separation normalized by the Einstein radius is s = 2.39 ± 0.05. There are three degenerate physical solutions and two of these are due to a new type of degeneracy in the microlensing parallax parameters, which we designate “the wide degeneracy.” The three models have (i) a Neptune-mass planet with a mass of

orbiting a low-mass M-dwarf with a mass of

, (ii) a mini-Neptune with

orbiting a brown dwarf host with

, and (iii) a super-Earth with

orbiting a low-mass brown dwarf host with

, which is slightly favored. The 3D planet–host separations are

au,

au, and

au, which are

,

, or

times larger than a
snow for these models, respectively. Keck adaptive optics observations confirm that the lens is faint. This discovery suggests that low-mass planets with Neptune-like orbits are common. Therefore processes similar to the one that formed Neptune in our own solar system or cold super-Earths may be common in other solar systems.
EMERGENCE OF GRANULAR-SIZED MAGNETIC BUBBLES THROUGH THE SOLAR ATMOSPHERE. III. THE PATH TO THE TRANSITION REGION
Authors: Ortiz Ada , Hansteen Viggo H. , Rubio Luis Ramón Bellot , Rodríguez Jaime de la Cruz , Pontieu Bart De , Carlsson Mats , Voort Luc Rouppe van der 
Published: July 2016

ABSTRACT
We study, for the first time, the ascent of granular-sized magnetic bubbles from the solar photosphere through the chromosphere into the transition region and above. Such events occurred in a flux emerging region in NOAA 11850 on 2013 September 25. During that time, the first co-observing campaign between the Swedish 1-m Solar Telescope (SST) and the Interface Region Imaging Spectrograph (IRIS) spacecraft was carried out. Simultaneous observations of the chromospheric Hα 656.28 nm and Ca ii 854.2 nm lines, plus the photospheric Fe i 630.25 nm line, were made with the CRISP spectropolarimeter at the Spitzer Space Telescope (SST) reaching a spatial resolution of 0.″14. At the same time, IRIS was performing a four-step dense raster of the emerging flux region, taking slit jaw images at 133 (C ii, transition region), 140 (Si iv, transition region), 279.6 (Mg ii k, core, upper chromosphere), and 283.2 nm (Mg ii k, wing, photosphere). Spectroscopy of several lines was performed by the IRIS spectrograph in the far- and near-ultraviolet, of which we have used the Si iv 140.3 and the Mg ii k 279.6 nm lines. Coronal images from the Atmospheric Imaging Assembly of the Solar Dynamics Observatory were used to investigate the possible coronal signatures of the flux emergence events. The photospheric and chromospheric properties of small-scale emerging magnetic bubbles have been described in detail in Ortiz et al. Here we are able to follow such structures up to the transition region. We describe the properties, including temporal delays, of the observed flux emergence in all layers. We believe this may be an important mechanism of transporting energy and magnetic flux from subsurface layers to the transition region and corona.