bluuebunny/crossref_metadata_2025_split huggingface dataset:
Twenty microsatellite markers for the endangered Vatica mangachapoi (Dipterocarpaceae)
Authors: Guo Jun‐Jie , Shang Shuai‐Bin , Wang Chun‐Sheng , Zhao Zhi‐Gang , Zeng Jie 
Published: February 2017

Premise of the study:Microsatellite markers were developed for Vatica mangachapoi (Dipterocarpaceae), an endangered species indigenous to Southeast Asia and southern China.Methods and Results:Twenty microsatellite markers, including 12 polymorphic markers, were identified from V. mangachapoi using high‐throughput sequencing. Polymorphism at each marker was evaluated using 87 individuals from three natural populations. The number of alleles per polymorphic locus ranged from six to 15, and the observed and expected heterozygosity varied from 0.000 to 0.926 and from 0.177 to 0.864, respectively. These markers were transferred successfully to the endangered species V. guangxiensis.Conclusions:These markers may be used to investigate the genetic diversity and gene flow of V. mangachapoi and V. guangxiensis.
Articulated Actions of the Family Health Strategy Teams and their Centres of Support in the State of Piauí, Brazil
Authors: Almeida Belas Izaias , Alves da Rocha Jorge Henrique , Melo da Silva Filipe , Batista Lustosa João Victor , Soares Carneiro Wendell , Gondim Valença Ana Maria , Saraiva da Silva Erisonval , Rodrigues Jailson Alberto 
Published: February 2017

Objective: From the perspective of professionals acting in the Family Health Strategy (FHS) in the state of Piauí, Brazil, the aim of this study was to asses the articulated actions of technical-pedagogical and clinical-care support offered by the Family Health Support Centres (FHSC) to the FHS’s professionals.
Methodology: This is an analytical census retrospective study, with a cross sectional design developed in a quantitative approach with a descriptive and exploratory nature. The research data was collected through the Program of Improvement in Quality of Access in Primary Care (PIAQ-PC) in Brazil, on its second cycle in 2013, and were analysed by using descriptive statistics.
Results: The actions of clinical-care support has been further developed by FHSC, all with frequency greater than 85%. In Piauí, the fields where FHSC has showed to be the nutritional care, rehabilitation and maternal and child care and also non-communicative diseases NCD that showed frequency higher than 85%.
Conclusion: The FHSC initiative contributes significantly with their services to the FHS to achieve its goals. However, to make the work of these teams more effective there must be ownership of Primary Care Services by its user and appreciation of it by the managers. The developed actions are being supported and agreed on among the matrix support teams.
Keywords: Primary Health Care; Health Promotion; Family Health.
Palliative Care To The Elderly Patient With Cancer: Speech Of Nurses
Authors: Carvalho da Silva Irany , Serpa de Souza Batista Patrícia , Carvalho dos Santos Platel Indiara , Da Costa Silv Jessyka Cibelly Minervina , Rodrigues Alves de Lima Débora , Alves da Silva Wiliana Aparecida , De Freitas Farias Priscilla , Bezerra da Rocha Alves Alany , Ferreira da Costa Thaíza , Sena de Lima Dereck , Jovino Borja Thayana 
Published: February 2017

Palliative care is aimed at people with diseases without perspective of cure or terminally, aiming to provide a better quality of life. This study aims to investigating the discourse of nurses about their understanding of palliative care to elderly patient with cancer and identify strategies used by nurses to promote palliative care to the elderly cancer patient. It is an exploratory research of a qualitative nature, carried out with thirteen nurses from a philanthropic institution in the city of João Pessoa, through a questionnaire.
The empirical material was subjected to thematic content analysis, resulting in three categories: design of nurses to assist the elderly in Palliative Care: promoting comfort and minimizing the suffering, the importance of palliative care in humanized care to the elderly with cancer and strategies for the Promotion of Care of the Elderly with Cancer.
Participants highlighted the palliative care as essential in the humanization of care, ensuring the dignity and quality of life among the elderly with cancer without possibilities of cure, adding such assistance, the family.
Keywords: Palliative Care; Nurse; Elderly; Cancer.
Global Energetics of Solar Flares. V. Energy Closure in Flares and Coronal Mass Ejections
Authors: Aschwanden Markus J. , Caspi Amir , Cohen Christina M. S. , Holman Gordon , Jing Ju , Kretzschmar Matthieu , Kontar Eduard P. , McTiernan James M. , Mewaldt Richard A. , O’Flannagain Aidan , Richardson Ian G. , Ryan Daniel , Warren Harry P. , Xu Yan 
Published: February 2017

Abstract
In this study we synthesize the results of four previous studies on the global energetics of solar flares and associated coronal mass ejections (CMEs), which include magnetic, thermal, nonthermal, and CME energies in 399 solar M- and X-class flare events observed during the first 3.5 yr of the Solar Dynamics Observatory (SDO) mission. Our findings are as follows. (1) The sum of the mean nonthermal energy of flare-accelerated particles (

), the energy of direct heating (

), and the energy in CMEs (

), which are the primary energy dissipation processes in a flare, is found to have a ratio of

, compared with the dissipated magnetic free energy

, which confirms energy closure within the measurement uncertainties and corroborates the magnetic origin of flares and CMEs. (2) The energy partition of the dissipated magnetic free energy is: 0.51 ± 0.17 in nonthermal energy of

electrons, 0.17 ± 0.17 in nonthermal

ions, 0.07 ± 0.14 in CMEs, and 0.07 ± 0.17 in direct heating. (3) The thermal energy is almost always less than the nonthermal energy, which is consistent with the thick-target model. (4) The bolometric luminosity in white-light flares is comparable to the thermal energy in soft X-rays (SXR). (5) Solar energetic particle events carry a fraction

of the CME energy, which is consistent with CME-driven shock acceleration. (6) The warm-target model predicts a lower limit of the low-energy cutoff at

, based on the mean peak temperature of the differential emission measure of T
e = 8.6 MK during flares. This work represents the first statistical study that establishes energy closure in solar flare/CME events.
Properties of Dense Cores Embedded in Musca Derived from Extinction Maps and 13CO, C18O, and NH3 Emission Lines
Authors: Machaieie Dinelsa A. , Vilas-Boas José W. , Wuensche Carlos A. , Racca Germán A. , Myers Philip C. , Hickel Gabriel R. 
Published: February 2017

Abstract
Using near-infrared data from the Two Micron All Sky Survey catalog and the Near Infrared Color Excess method, we studied the extinction distribution in five dense cores of Musca, which show visual extinction greater than 10 mag and are potential sites of star formation. We analyzed the stability in four of them, fitting their radial extinction profiles with Bonnor–Ebert isothermal spheres, and explored their properties using the J = 1–0 transition of 13CO and C18O and the J = K = 1 transition of NH3. One core is not well described by the model. The stability parameter of the fitted cores ranges from 4.5 to 5.7 and suggests that all cores are stable, including Mu13, which harbors one young stellar object (YSO), the IRAS 12322-7023 source. However, the analysis of the physical parameters shows that Mu13 tends to have larger A
V, n
c, and P
ext than the remaining starless cores. The other physical parameters do not show any trend. It is possible that those are the main parameters to explore in active star-forming cores. Mu13 also shows the most intense emission of NH3. Its 13CO and C18O lines have double peaks, whose integrated intensity maps suggest that they are due to the superposition of clouds with different radial velocities seen in the line of sight. It is not possible to state whether these clouds are colliding and inducing star formation or are related to a physical process associated with the formation of the YSO.
Pale Orange Dots: The Impact of Organic Haze on the Habitability and Detectability of Earthlike Exoplanets
Authors: Arney Giada N. , Meadows Victoria S. , Domagal-Goldman Shawn D. , Deming Drake , Robinson Tyler D. , Tovar Guadalupe , Wolf Eric T. , Schwieterman Edward 
Published: February 2017

Abstract
Hazes are common in known planetary atmospheres, and geochemical evidence suggests that early Earth occasionally supported an organic haze with significant environmental and spectral consequences. The UV spectrum of the parent star drives organic haze formation through methane photochemistry. We use a 1D photochemical-climate model to examine production of fractal organic haze on Archean Earth-analogs in the habitable zones of several stellar types: the modern and early Sun, AD Leo (M3.5V), GJ 876 (M4V), ϵ Eridani (K2V), and σ Boötis (F2V). For Archean-like atmospheres, planets orbiting stars with the highest UV fluxes do not form haze because of the formation of photochemical oxygen radicals that destroy haze precursors. Organic hazes impact planetary habitability via UV shielding and surface cooling, but this cooling is minimized around M dwarfs, whose energy is emitted at wavelengths where organic hazes are relatively transparent. We generate spectra to test the detectability of haze. For 10 transits of a planet orbiting GJ 876 observed by the James Webb Space Telescope, haze makes gaseous absorption features at wavelengths < 2.5 μm 2–10σ shallower than a haze-free planet, and methane and carbon dioxide are detectable at >5σ. A haze absorption feature can be detected at 5σ near 6.3 μm, but a higher signal-to-noise ratio is needed to distinguish haze from adjacent absorbers. For direct imaging of a planet at 10 pc using a coronagraphic 10 m class ultraviolet–visible–near-infrared telescope, a UV–blue haze absorption feature would be strongly detectable at >12σ in 200 hr.
The X-Ray Binary Population of the Nearby Dwarf Starburst Galaxy IC 10: Variable and Transient X-Ray Sources
Authors: Laycock Silas , Cappallo Rigel , Williams Benjamin F. , Prestwich Andrea , Binder Breanna , Christodoulou Dimitris M. 
Published: February 2017

Abstract
We have monitored the Cassiopeia dwarf galaxy (IC 10) in a series of 10 Chandra ACIS-S observations to capture its variable and transient X-ray source population, which is expected to be dominated by High Mass X-ray Binaries (HMXBs). We present a sample of 21 X-ray sources that are variable between observations at the 3σ level, from a catalog of 110 unique point sources. We find four transients (flux variability ratio greater than 10) and a further eight objects with ratios >5. The observations span the years 2003–2010 and reach a limiting luminosity of >1035 erg s−1, providing sensitivity to X-ray binaries in IC 10 as well as flare stars in the foreground Milky Way. The nature of the variable sources is investigated from light curves, X-ray spectra, energy quantiles, and optical counterparts. The purpose of this study is to discover the composition of the X-ray binary population in a young starburst environment. IC 10 provides a sharp contrast in stellar population age (<10 My) when compared to the Magellanic Clouds (40–200 My) where most of the known HMXBs reside. We find 10 strong HMXB candidates, 2 probable background Active Galactic Nuclei, 4 foreground flare-stars or active binaries, and 5 not yet classifiable sources. Complete classification of the sample requires optical spectroscopy for radial velocity analysis and deeper X-ray observations to obtain higher S/N spectra and search for pulsations. A catalog and supporting data set are provided.
Testing the Large-scale Environments of Cool-core and Non-cool-core Clusters with Clustering Bias
Authors: Medezinski Elinor , Battaglia Nicholas , Coupon Jean , Cen Renyue , Gaspari Massimo , Strauss Michael A. , Spergel David N. 
Published: February 2017

Abstract
There are well-observed differences between cool-core (CC) and non-cool-core (NCC) clusters, but the origin of this distinction is still largely unknown. Competing theories can be divided into internal (inside-out), in which internal physical processes transform or maintain the NCC phase, and external (outside-in), in which the cluster type is determined by its initial conditions, which in turn leads to different formation histories (i.e., assembly bias). We propose a new method that uses the relative assembly bias of CC to NCC clusters, as determined via the two-point cluster-galaxy cross-correlation function (CCF), to test whether formation history plays a role in determining their nature. We apply our method to 48 ACCEPT clusters, which have well resolved central entropies, and cross-correlate with the SDSS-III/BOSS LOWZ galaxy catalog. We find that the relative bias of NCC over CC clusters is b = 1.42 ± 0.35 (1.6σ different from unity). Our measurement is limited by the small number of clusters with core entropy information within the BOSS footprint, 14 CC and 34 NCC clusters. Future compilations of X-ray cluster samples, combined with deep all-sky redshift surveys, will be able to better constrain the relative assembly bias of CC and NCC clusters and determine the origin of the bimodality.
An Exploration of Heating Mechanisms in a Supra-arcade Plasma Sheet Formed after a Coronal Mass Ejection
Authors: Reeves Katharine K. , Freed Michael S. , McKenzie David E. , Savage Sabrina L. 
Published: February 2017

Abstract
We perform a detailed analysis of the thermal structure of the region above the post-eruption arcade for a flare that occurred on 2011 October 22. During this event, a sheet of hot plasma is visible above the flare loops in the 131 Å bandpass of the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory. Supra-arcade downflows (SADs) are observed traveling sunward through the post-eruption plasma sheet. We calculate differential emission measures using the AIA data and derive an emission measure weighted average temperature in the supra-arcade region. In areas where many SADs occur, the temperature of the supra-arcade plasma tends to increase, while in areas where no SADs are observed, the temperature tends to decrease. We calculate the plane-of-sky velocities in the supra-arcade plasma and use them to determine the potential heating due to adiabatic compression and viscous heating. Of the 13 SADs studied, 10 have noticeable signatures in both the adiabatic and the viscous terms. The adiabatic heating due to compression of plasma in front of the SADs is on the order of 0.1–0.2 MK/s, which is similar in magnitude to the estimated conductive cooling rate. This result supports the notion that SADs contribute locally to the heating of plasma in the supra-arcade region. We also find that in the region without SADs, the plasma cools at a rate that is slower than the estimated conductive cooling, indicating that additional heating mechanisms may act globally to keep the plasma temperature high.
First Measurement of the 19F(α, p)22Ne Reaction at Energies of Astrophysical Relevance
Authors: Pizzone R. G. , D’Agata G. , Cognata M. La , Indelicato I. , Spitaleri C. , Blagus S. , Cherubini S. , Figuera P. , Grassi L. , Guardo G. L. , Gulino M. , Hayakawa S. , Kshetri R. , Lamia L. , Lattuada M. , Mijatović T. , Milin M. , Miljanić D. Đ. , Prepolec L. , Rapisarda G. G. , Romano S. , Sergi M. L. , Skukan N. , Soić N. , Tokić V. , Tumino A. , Uroić M. 
Published: February 2017

Abstract
The observational 19F abundance in stellar environments systematically exceeds the predicted one, thus representing one of the unsolved challenges for stellar modeling. It is therefore clear that further investigation is needed in this field. In this work, we focus our attention on the measurement of the

reaction in the astrophysical energy range, between 0.2 and 0.8 MeV (far below the Coulomb barrier, 3.8 MeV), as it represents the main destruction channel in He-rich environments. The lowest energy at which this reaction has been studied with direct measurements is ∼0.66 MeV, covering only the upper tail of the Gamow window, causing the reaction-rate evaluation to be based on extrapolation. To investigate lower energies, the

reaction has been studied by means of the Trojan horse method, applied to the quasi-free

reaction at E
beam = 6 MeV. The indirect cross section of the

reaction at energies ≲1 MeV was extracted, fully covering the astrophysical region of interest and overlapping existing direct data for normalization. Several resonances have been detected for the first time inside the Gamow window. The reaction rate has been calculated, showing an increase up to a factor of 4 with respect to the literature at astrophysical temperatures. This might lead to potential major astrophysical implications.
A Search for Interstellar Monohydric Thiols
Authors: Gorai Prasanta , Das Ankan , Das Amaresh , Sivaraman Bhalamurugan , Etim Emmanuel E. , Chakrabarti Sandip K. 
Published: February 2017

Abstract
It has been pointed out by various astronomers that a very interesting relationship exists between interstellar alcohols and the corresponding thiols (sulfur analog of alcohols) as far as the spectroscopic properties and chemical abundances are concerned. Monohydric alcohols such as methanol and ethanol are widely observed and 1-propanol was recently claimed to have been seen in Orion KL. Among the monohydric thiols, methanethiol (chemical analog of methanol) has been firmly detected in Orion KL and Sgr B2(N2) and ethanethiol (chemical analog of ethanol) has been observed in Sgr B2(N2), though the confirmation of this detection is yet to come. It is very likely that higher order thiols could be observed in these regions. In this paper, we study the formation of monohydric alcohols and their thiol analogs. Based on our quantum chemical calculation and chemical modeling, we find that the Tg conformer of 1-propanethiol is a good candidate of astronomical interest. We present various spectroscopically relevant parameters of this molecule to assist in its future detection in the interstellar medium.
Polarization Radiation with Turbulent Magnetic Fields from X-Ray Binaries
Authors: Zhang (张建福) Jian-Fu , Xiang (向福元) Fu-Yuan , Lu (卢炬甫) Ju-Fu 
Published: February 2017

Abstract
We study the properties of polarized radiation in turbulent magnetic fields from X-ray binary jets. These turbulent magnetic fields are composed of large- and small-scale configurations, which result in the polarized jitter radiation when the characteristic length of turbulence is less than the non-relativistic Larmor radius. On the contrary, the polarized synchrotron emission occurs, corresponding to a large-scale turbulent environment. We calculate the spectral energy distributions and the degree of polarization for a general microquasar. Numerical results show that turbulent magnetic field configurations can indeed provide a high degree of polarization, which does not mean that a uniform, large-scale magnetic field structure exists. The model is applied to investigate the properties of polarized radiation of the black-hole X-ray binary Cygnus X-1. Under the constraint of multiband observations of this source, our studies demonstrate that the model can explain the high polarization degree at the MeV tail and predict the highly polarized properties at the high-energy γ-ray region, and that the dominant small-scale turbulent magnetic field plays an important role for explaining the highly polarized observation at hard X-ray/soft γ-ray bands. This model can be tested by polarization observations of upcoming polarimeters at high-energy γ-ray bands.
Time-dependent Cooling in Photoionized Plasma
Authors: Gnat Orly 
Published: February 2017

Abstract
I explore the thermal evolution and ionization states in gas cooling from an initially hot state in the presence of external photoionizing radiation. I compute the equilibrium and nonequilibrium cooling efficiencies, heating rates, and ion fractions for low-density gas cooling while exposed to the ionizing metagalactic background radiation at various redshifts (z = 0 − 3), for a range of temperatures (108–104 K), densities (10−7–103 cm−3), and metallicities (10−3–2 times solar). The results indicate the existence of a threshold ionization parameter, above which the cooling efficiencies are very close to those in photoionization equilibrium (so that departures from equilibrium may be neglected), and below which the cooling efficiencies resemble those in collisional time-dependent gas cooling with no external radiation (and are thus independent of density).
Astrochemical Properties of Planck Cold Clumps
Authors: Tatematsu Ken’ichi , Liu Tie , Ohashi Satoshi , Sanhueza Patricio , Nguyễn Lu’o’ng Quang , Hirota Tomoya , Liu Sheng-Yuan , Hirano Naomi , Choi Minho , Kang Miju , A.Thompson Mark , Fuller Gary , Wu Yuefang , Li Di , Francesco James Di , Kim Kee-Tae , Wang Ke , Ristorcelli Isabelle , Juvela Mika , Shinnaga Hiroko , Cunningham Maria , Saito Masao , Lee Jeong-Eun , Tóth L. Viktor , He Jinhua , Sakai Takeshi , Kim Jungha ,   (JCMT Large Program “SCOPE” collaboration),   (TRAO Key Science Program “TOP” collaboration)
Published: February 2017

Abstract
We observed 13 Planck cold clumps with the James Clerk Maxwell Telescope/SCUBA-2 and with the Nobeyama 45 m radio telescope. The N2H+ distribution obtained with the Nobeyama telescope is quite similar to SCUBA-2 dust distribution. The 82 GHz HC3N, 82 GHz CCS, and 94 GHz CCS emission are often distributed differently with respect to the N2H+ emission. The CCS emission, which is known to be abundant in starless molecular cloud cores, is often very clumpy in the observed targets. We made deep single-pointing observations in DNC, HN13C, N2D+, and cyclic-C3H2 toward nine clumps. The detection rate of N2D+ is 50%. Furthermore, we observed the NH3 emission toward 15 Planck cold clumps to estimate the kinetic temperature, and confirmed that most targets are cold (≲20 K). In two of the starless clumps we observed, the CCS emission is distributed as it surrounds the N2H+ core (chemically evolved gas), which resembles the case of L1544, a prestellar core showing collapse. In addition, we detected both DNC and N2D+. These two clumps are most likely on the verge of star formation. We introduce the chemical evolution factor (CEF) for starless cores to describe the chemical evolutionary stage, and analyze the observed Planck cold clumps.
Challenges to Constraining Exoplanet Masses via Transmission Spectroscopy
Authors: Batalha Natasha E. , Kempton Eliza M.-R. , Mbarek Rostom 
Published: February 2017

Abstract

MassSpec, a method for determining the mass of a transiting exoplanet from its transmission spectrum alone, was proposed by de Wit & Seager. The premise of this method relies on the planet’s surface gravity being extracted from the transmission spectrum via its effect on the atmospheric scale height, which in turn determines the strength of absorption features. Here, we further explore the applicability of MassSpec to low-mass exoplanets—specifically those in the super-Earth size range for which radial velocity determinations of the planetary mass can be extremely challenging and resource intensive. Determining the masses of these planets is of the utmost importance because their nature is otherwise highly unconstrained. Without knowledge of the mass, these planets could be rocky, icy, or gas-dominated. To investigate the effects of planetary mass on transmission spectra, we present simulated observations of super-Earths with atmospheres made up of mixtures of H2O and H2, both with and without clouds. We model their transmission spectra and run simulations of each planet as it would be observed with James Webb Space Telescope using the NIRISS, NIRSpec, and MIRI instruments. We find that significant degeneracies exist between transmission spectra of planets with different masses and compositions, making it impossible to unambiguously determine the planet’s mass in many cases.