bluuebunny/crossref_metadata_2025_split huggingface dataset:
Traditional honey harvesting by the Pnar community of South Assam, India
Authors: Deori Biswajyoti Bikomiya , Deb Panna , Singha Hilloljyoti , Choudhury Manabendra Ray 
Published: January 2017

Honey obtained from the bee hives is a sweet food and has a great medicinal value. Honey collected from nature by the ethnic communities is an important source of nutrition and also contribute to their income generation. Honey collection from the wild is especially done by the indigenous tribe and forest dwellers. The Pnar community living in Barak Valley, South Assam is also engaged in the collection of honey from the forest, especially during the spring season. The process starts with the gathering of information, followed by the preparation for the activity and subsequently extraction of honey from the bee hive. The technique used by the Pnar community is a challenging one as it involves harvesting of honey from lofty trees in forest with traditionally made gears like bamboo basket, smoke torch and a one bamboo ladder. The indigenous ways involves lining the bamboo basket with leaves for the collection of honey, using smoke to frighten the bee and storage of honey in the bamboo pipes. The present study exhibits the rich traditional knowledge that has paved the way for a sustainable livelihood since long and at the same time provides income generation opportunity for the community. This work is licensed under a Creative Commons Attribution-NonCommercial 4.0 International License.
Epidemiological study of clinical signs and symptoms of mercury poisoning in fish consumers residing in five villages along Thane Creek and Ulhas River Estuary near Mumbai, India
Authors: Menon Jayashree S. 
Published: January 2017

The fish of Thane Creek and Ulhas River Estuary are contaminated with mercury. The traditional fishing folks residing along these water sources consume large amounts of these fish for their sustenance, therefore, being vulnerable to mercury poisoning. A survey on the clinical signs and symptoms of mercury poisoning was carried out in Wehele, Alimgarh and Diwe-Kewni along Ulhas River Estuary and Vittawa and Airoli along Thane creek. Fortunately, no alarming signals of mercury poisoning could be detected in these populations. Genetic make-up and/or use of onion and garlic in the fish preparations could be the probable detoxifying factors in these populations. However, these populations being vulnerable to mercury poisoning, continuous monitoring is recommended in these areas. This work is licensed under a Creative Commons Attribution-NonCommercial 4.0 International License.
Water quality and red bloom algae of fish ponds in three different regions of Nepal
Authors: Mandal Ram Bhajan , Rai Sunila , Shrestha Madhav Kumar , Jha Dilip Kumar , Pandit Narayan Prasad , Rai Shiva Kumar 
Published: January 2017

Present study determines the causes and seasonal variation of red bloom in fishponds of Eastern, Western and Central regions of Nepal. Monthly monitoring of water quality and phytoplankton was carried out for one year. Water parameters such as NH3-N, total phosphorus, total Kjeldahl nitrogen (TKN), total dissolved solids (TDS) and conductivity were significantly higher (p<0.05) in red bloom fishponds than non-red bloom fishponds. The total density of euglenophytes in red-bloom fishponds was significantly higher (P<0.05) (1970±260 cells L-1) than non-red bloom fishponds (410±30 cells L-1). Euglenophyte density varied seasonally and significantly lower in spring season (1250±220 cells L-1) than autumn (1950±390 cells L-1), winter (2180±370 cells L-1), and summer (2490±480 cells L-1) in red bloom fishponds. High nutrients might favor the growth of euglenophytes (Euglena sanguinea) causing red bloom fish ponds of Nepal. This work is licensed under a Creative Commons Attribution-NonCommercial 4.0 International License.
GPs’ perceptions of workload in England: a qualitative interview study
Authors: Croxson Caroline HD , Ashdown Helen F , Hobbs FD Richard 
Published: January 2017

BackgroundGPs report the lowest levels of morale among doctors, job satisfaction is low, and the GP workforce is diminishing. Workload is frequently cited as negatively impacting on commitment to a career in general practice, and many GPs report that their workload is unmanageable.AimTo gather an in-depth understanding of GPs’ perceptions and attitudes towards workload.Design and settingAll GPs working within NHS England were eligible. Advertisements were circulated via regional GP e-mail lists and national social media networks in June 2015. Of those GPs who responded, a maximum-variation sample was selected until data saturation was reached.MethodSemi-structured, qualitative interviews were conducted. Data were analysed thematically.ResultsIn total, 171 GPs responded, and 34 were included in this study. GPs described an increase in workload over recent years, with current working days being long and intense, raising concerns over the wellbeing of GPs and patients. Full-time partnership was generally not considered to be possible, and many participants felt workload was unsustainable, particularly given the diminishing workforce. Four major themes emerged to explain increased workload: increased patient needs and expectations; a changing relationship between primary and secondary care; bureaucracy and resources; and the balance of workload within a practice. Continuity of care was perceived as being eroded by changes in contracts and working patterns to deal with workload.ConclusionThis study highlights the urgent need to address perceived lack of investment and clinical capacity in general practice, and suggests that managing patient expectations around what primary care can deliver, and reducing bureaucracy, have become key issues, at least until capacity issues are resolved.
Directly Observing the Galaxies Likely Responsible for Reionization
Authors: Livermore R. C. , Finkelstein S. L. , Lotz J. M. 
Published: January 2017

Abstract
We report a new analysis of the Hubble Frontier Fields clusters Abell 2744 and MACS 0416 using wavelet decomposition to remove the cluster light, enabling the detection of highly magnified (>50×) galaxies a factor of 10× fainter in luminosity than previous studies. We find 167 galaxies at

, and with this sample we are able to characterize the UV luminosity function to

at

, −14 at

, and −15 at

. We find a steep faint-end slope (

), and with our improved statistics at the faint end we reduce the fractional uncertainty on α to

at

and 4% at

. We also investigate the systematic uncertainty due to the lens modeling by using every available lens model individually and comparing the results; this systematic fractional uncertainty on α is

at all redshifts. We now directly observe galaxies in the luminosity regime where some simulations predict a change in the faint-end slope of the luminosity function, yet our results provide statistically very strong evidence against any turnover in the luminosity range probed, more consistent with simulations in which stars form in lower-mass halos. Thus, we find strong support for the extension of the steep luminosity function to

at

, consistent with the number of faint galaxies needed to reionize the universe under standard assumptions.
Rosseland and Flux Mean Opacities for Compton Scattering
Authors: Poutanen Juri 
Published: January 2017

Abstract
Rosseland mean opacity plays an important role in theories of stellar evolution and X-ray burst models. In the high-temperature regime, when most of the gas is completely ionized, the opacity is dominated by Compton scattering. Our aim here is to critically evaluate previous works on this subject and to compute the exact Rosseland mean opacity for Compton scattering over a broad range of temperature and electron degeneracy parameter. We use relativistic kinetic equations for Compton scattering and compute the photon mean free path as a function of photon energy by solving the corresponding integral equation in the diffusion limit. As a byproduct we also demonstrate the way to compute photon redistribution functions in the case of degenerate electrons. We then compute the Rosseland mean opacity as a function of temperature and electron degeneracy and present useful approximate expressions. We compare our results to previous calculations and find a significant difference in the low-temperature regime and strong degeneracy. We then proceed to compute the flux mean opacity in both free-streaming and diffusion approximations, and show that the latter is nearly identical to the Rosseland mean opacity. We also provide a simple way to account for the true absorption in evaluating the Rosseland and flux mean opacities.
Analysis of Low Excitation HDO Transitions toward the High-mass Star-forming Regions G34.26+0.15, W51e1/e2, and W49N
Authors: Kulczak-Jastrzȩbska Magda 
Published: January 2017

Abstract
We present observations of the ground state 10,1–00,0 rotational transition of HDO at 464.925 GHz and the 11,0–10,1 transition at 509.292 GHz, toward three high-mass star-forming regions: G34.26+0.15, W49N, and W51e1/e2, carried out with the Caltech Submillimeter Observatory. For the first time, the latter transition is observed from the ground. The spectra are modeled, together with observations of higher-energy HDO transitions, as well as submillimeter dust continuum fluxes from the literature, using a spherically symmetric radiative transfer model to derive the radial distribution of the HDO abundance in the target sources. The abundance profile is divided into an inner hot core region, with kinetic temperatures higher than 100 K, and a cold outer envelope with lower kinetic temperatures. The derived HDO abundance with respect to H2 is (0.3–3.7) × 10−8 in the hot inner region (T > 100 K) and (7.0–10.0) × 10−11 in the cold outer envelope. We also used two

fundamental transitions to constrain the H2O abundances in the outer envelopes. The HDO/H2O ratios in these cold regions are found to be (1.8–3.1) × 10−3 and consequently are higher than in the hot inner regions of these sources.
New Solar Irradiance Measurements from the Miniature X-Ray Solar Spectrometer Cubesat
Authors: Woods Thomas N. , Caspi Amir , Chamberlin Phillip C. , Jones Andrew , Kohnert Richard , Mason James Paul , Moore Christopher S. , Palo Scott , Rouleau Colden , Solomon Stanley C. , Machol Janet , Viereck Rodney 
Published: January 2017

Abstract
The goal of the Miniature X-ray Solar Spectrometer (MinXSS) CubeSat is to explore the energy distribution of soft X-ray (SXR) emissions from the quiescent Sun, active regions, and during solar flares and to model the impact on Earth's ionosphere and thermosphere. The energy emitted in the SXR range (0.1–10 keV) can vary by more than a factor of 100, yet we have limited spectral measurements in the SXRs to accurately quantify the spectral dependence of this variability. The MinXSS primary science instrument is an Amptek, Inc. X123 X-ray spectrometer that has an energy range of 0.5–30 keV with a nominal 0.15 keV energy resolution. Two flight models have been built. The first, MinXSS-1, has been making science observations since 2016 June 9 and has observed numerous flares, including more than 40 C-class and 7 M-class flares. These SXR spectral measurements have advantages over broadband SXR observations, such as providing the capability to derive multiple-temperature components and elemental abundances of coronal plasma, improved irradiance accuracy, and higher resolution spectral irradiance as input to planetary ionosphere simulations. MinXSS spectra obtained during the M5.0 flare on 2016 July 23 highlight these advantages and indicate how the elemental abundance appears to change from primarily coronal to more photospheric during the flare. MinXSS-1 observations are compared to the Geostationary Operational Environmental Satellite (GOES) X-ray Sensor (XRS) measurements of SXR irradiance and estimated corona temperature. Additionally, a suggested improvement to the calibration of the GOES XRS data is presented.
Globular Clusters as Tracers of Fine Structure in the Dramatic Shell Galaxy NGC 474
Authors: Lim Sungsoon , Peng Eric W. , Duc Pierre-Alain , Fensch Jérémy , Durrell Patrick R. , Harris William E. , Cuillandre Jean-Charles , Gwyn Stephen , Lançon Ariane , Sánchez-Janssen Rúben 
Published: January 2017

Abstract
Globular clusters (GCs) are some of the most visible tracers of the merging and accretion histories of galaxy halos. Metal-poor GCs, in particular, are thought to arrive in massive galaxies largely through dry, minor merging events, but it is rare to see a direct connection between GCs and visible stellar streams. NGC 474 is a post-merger early-type galaxy with dramatic fine structures made of concentric shells and radial streams that have been more clearly revealed by deep imaging. We present a study of GCs in NGC 474 to better establish the relationship between merger-induced fine structure and the GC system. We find that many GCs are superimposed on visible streams and shells, and about 35% of GCs outside

are located in regions of fine structure. The spatial correlation between GCs and fine structure is significant at the 99.9% level, which shows that this correlation is not coincidental. The colors of GCs on fine structures are mostly blue, and we also find an intermediate-color population that is dominant in the central region and that will likely passively evolve to have colors consistent with a traditional metal-rich GC population. The association of the blue GCs with fine structures is direct confirmation that many metal-poor GCs are accreted onto massive galaxy halos through merging events and that the progenitors of these mergers are sub-

galaxies.
Polarization Signatures of Kink Instabilities in the Blazar Emission Region from Relativistic Magnetohydrodynamic Simulations
Authors: Zhang Haocheng , Li Hui , Guo Fan , Taylor Greg 
Published: January 2017

Abstract
Kink instabilities are likely to occur in the current-carrying magnetized plasma jets. Recent observations of the blazar radiation and polarization signatures suggest that the blazar emission region may be considerably magnetized. While the kink instability has been studied with first-principle magnetohydrodynamic (MHD) simulations, the corresponding time-dependent radiation and polarization signatures have not been investigated. In this paper, we perform comprehensive polarization-dependent radiation modeling of the kink instability in the blazar emission region based on relativistic MHD (RMHD) simulations. We find that the kink instability may give rise to strong flares with polarization angle (PA) swings or weak flares with polarization fluctuations, depending on the initial magnetic topology and magnetization. These findings are consistent with observations. Compared with the shock model, the kink model generates polarization signatures that are in better agreement with the general polarization observations. Therefore, we suggest that kink instabilities may widely exist in the jet environment and provide an efficient way to convert the magnetic energy and produce multiwavelength flares and polarization variations.
Observations of the Formation, Development, and Structure of a Current Sheet in an Eruptive Solar Flare
Authors: Seaton Daniel B. , Bartz Allison E. , Darnel Jonathan M. 
Published: January 2017

Abstract
We present Atmospheric Imaging Assembly observations of a structure we interpret as a current sheet associated with an X4.9 flare and coronal mass ejection that occurred on 2014 February 25 in NOAA Active Region 11990. We characterize the properties of the current sheet, finding that the sheet remains on the order of a few thousand kilometers thick for much of the duration of the event and that its temperature generally ranged between 8 and 10 MK. We also note the presence of other phenomena believed to be associated with magnetic reconnection in current sheets, including supra-arcade downflows and shrinking loops. We estimate that the rate of reconnection during the event was M

A
≈ 0.004–0.007, a value consistent with model predictions. We conclude with a discussion of the implications of this event for reconnection-based eruption models.
L1188: A Promising Candidate for Cloud–Cloud Collisions Triggering the Formation of Low- and Intermediate-mass Stars
Authors: Gong Yan , Fang Min , Mao Ruiqing , Zhang Shaobo , Wang Yuan , Su Yang , Chen Xuepeng , Yang Ji , Wang Hongchi , Lu Dengrong 
Published: January 2017

Abstract
We present a new large-scale (2° × 2°) simultaneous 12CO, 13CO, and C18O (J = 1–0) mapping of L1188 with the Purple Mountain Observatory 13.7 m telescope. Our observations have revealed that L1188 consists of two nearly orthogonal filamentary molecular clouds at two clearly separated velocities. Toward the intersection showing large velocity spreads, we find several bridging features connecting the two clouds in velocity, and an open arc structure that exhibits high excitation temperatures, enhanced 12CO and 13CO emission, and broad 12CO line wings. This agrees with the scenario that the two clouds are colliding with each other. The distribution of young stellar object (YSO) candidates implies an enhancement of star formation in the intersection of the two clouds. We suggest that a cloud–cloud collision happened in L1188 about 1 Myr ago, possibly triggering the formation of low- and intermediate-mass YSOs in the intersection.
Particle-in-cell Simulations of Electron and Ion Dissipation by Whistler Turbulence: Variations with Electron β
Authors: Hughes R. Scott , Gary S. Peter , Wang Joseph 
Published: January 2017

Abstract
Two ensembles of three-dimensional particle-in-cell (PIC) simulations of the forward cascade of decaying whistler turbulence have been carried out on a model of collisionless, homogeneous, magnetized plasma with parameters similar to those of the solar wind near Earth. Initial, relatively isotropic, narrowband spectra of relatively long wavelength modes cascade to anisotropic, broadband spectra of magnetic fluctuations at shorter wavelengths. Electron and ion dissipation rates are computed as functions of the initial electron beta, β
e, over the range 0.1 ≤ β
e ≤ 5.0, where this quantity is varied by changes in the background magnetic field magnitude B
o. Ensemble One holds the value of the dimensionless initial magnetic fluctuation energy density ϵ
o ≡ Σk

constant; Ensemble Two follows solar wind observations, imposing the initial condition ϵ
o = 0.20 β
e. In both ensembles, the maximum dissipation rate of the electrons, Q
e, and the maximum dissipation rate of the ions, Q
i, satisfy Q
e ≫ Q
i. In Ensemble One, both dissipation rates scale approximately as

, whereas over 0.1 ≤ β
e ≤ 1.0 in Ensemble Two, Q
e is approximately constant while Q
i scales approximately as

. These results, when combined with conclusions from earlier PIC simulations, suggest that sufficiently long wavelength and sufficiently large-amplitude magnetosonic-whistler turbulence at sufficiently large β
e may heat ions more rapidly than electrons.
The Local Spiral Arm in the LAMOST-Gaia Common Stars?
Authors: Liu Chao , Wang You-Gang , Shen Juntai , Li Zhao-Yu , Qin Yu-Jing , Hou Yonghui , Wang Yuefei , Zhang Yong , Cao Zihuang , Wu Yue 
Published: January 2017

Abstract
Using the LAMOST-Gaia common stars, we demonstrate that the in-plane velocity fields for the nearby young stars are significantly different from those for the old ones. For the young stars, the probably perturbed velocities that are similar to the old population are mostly removed from the velocity maps in the X–Y plane. The residual velocity field shows that the young stars consistently move along Y with faster v

ϕ
at the trailing side of the local arm, while at the leading side, they move slower in the azimuth direction. At both sides, on average the young stars move inward with a v

R
of

km s−1. The divergence of the velocity in the Y direction implies that the young stars are associated with a density wave near the local arm. We therefore suggest that the young stars may reflect the formation of the local spiral arm by correlating themselves with a density wave. The range of the age for the young stars is around 2 Gyr, which is sensible since the transient spiral arm can persist for that long. We also point out that alternative explanations of the peculiar velocity field for the young population cannot be ruled out if solely using this observed data.
Psychophysiological analysis of Kriya Yoga as per Patanjala Yoga Sutra
Authors: Bapat Sarita Vivek 
Published: January 2017

Background:
Kriya Yoga that includes Tapas,vadhyaya, and Ishwara pranidhana as given by Patanjala Yoga Sutra finds its mention twice in the text as Kriya Yoga and as Niyama. The double occurrence has significance.

Aim:
The aim of this work is to carry out an analysis of what Kriya Yoga is, what is the purpose of repeating three components of Kriya Yoga, i.e., Tapas,vadhyaya, and Ishwara pranidhana in Sadhana pada.

Method:
The three steps of Tapas,Svadhyaya, and Ishwara pranidhana were analyzed in detail. The important difference of this analysis from other commentators is to analyze the first two steps of Kriya Yoga from the psychophysiological point of view.

Analysis:
The Kriya Yoga brings psychophysiological changes leading to the total control of the body, i.e., internal functions of the body. It also leads to surrender to the internal supreme existence of one's own being. The process of Tapas, Svadhyaya, and Ishwara pranidhana, as per Kriya Yoga, converts a common person into a yogi.

Conclusion:
The process of Kriya Yoga facilitates the removal of resistance within i.e. preparing condition of chitta which is necessary for entering into Samadhi is fulfilled.
New light on Kliṣṭa and Akliṣṭa Vrttis
Authors: Mahadevan Jayaraman 
Published: January 2017

Context:
Patañjali Yoga Sūtras classify Citta Vrttis into the Kliṣṭa and Akliṣṭa (Desikachar, 2014, p.16). After this initial mention, there are no further discussions on this 2-fold classification of the Vrttis in the text. Though Kleśas are discussed in the second chapter of text, the terms Kliṣṭa and Akliṣṭa themselves do not appear as part of discussion in the entire text after this initial mention. This gives rise to quite a few questions: What is the purpose of classifying the Vrttis into Kliṣṭa and Akliṣṭa? What is meant by Kliṣṭa and Akliṣṭa Vrttis? What is the nature of association of Kleśas with Vrttis? Should both Kliṣṭa and Akliṣṭa Vrttis be restrained or will it be enough if one focuses on restraining the Kliṣṭa Vrttis? and so on.

Aim:
Though the Sūtras themselves do not reveal any further information on this, many Sanskrit commentaries of Yoga Sūtra, beginning from the one ascribed to Vyāsa, address these questions. The aim is to study these commentaries to find answers to the questions raised above.

Method:
A descriptive method of analyzing arguments is used because of the philosophico-literary nature of the study.

Result:
The commentaries along with presenting various possible answers to the questions on the Kliṣṭa and Akliṣṭa Vrttis of the Yoga sūtras also reveal more relevant insights.

Conclusion:
On scrutiny of the commentaries, it becomes evident that all the techniques of Patañjali in the Yoga Sūtras, be it Abhyāsa vairagya, Kriyā Yoga, or Aṣṭāṅga Yoga, operate on the principles discussed under the Sūtra on Kliṣṭa and Akliṣṭa classification establishing Kliṣṭa and Akliṣṭa Vrttis as the foundational principles of Yoga Sūtras. The diverse yogic methods and techniques that are prescribed centered onthe body, breath, emotions, intellect, etc., seem to be aimed only at the generation of progressively varying levels of Akliṣṭa Vrttis and ultimately to overcome even these Akliṣṭa Vrttis to attain absolute Citta-vritti-nirodha.