bluuebunny/crossref_metadata_2025_split huggingface dataset:
Nurse prescribing in primary care: a metasynthesis of the literature
Authors: Nuttall Dilyse 
Published: August 2017

Aim
The aim of this metasynthesis was to develop an understanding of the existing theoretical perspectives around nurse prescribing and to identify any gaps in knowledge, which would support further research into the lived experience of the nurse prescriber in the primary care setting.

Background
Nurse prescribing has been the focus of many research studies since its introduction, with many benefits to the patient, the prescriber and service identified; however, there remains variation in the utilisation of the prescribing qualification, particularly in primary care settings. Although a range of quantitative and qualitative studies have been undertaken, which aimed to explore the influences on prescribing, few have used a research methodology that supports the in-depth exploration of the nurse prescriber’s experience.

Methods
An extensive literature search was undertaken in April 2015 (20–24), which included UK and non-UK studies since 1999. Inclusion and exclusion criteria were applied to search for studies in which participants included nurse prescribers who practiced in primary or community care settings. Studies that only used a quantitative methodology and those not available in English were excluded. The literature search yielded 124 papers, with 50 papers remaining after the initial screen of full papers against the inclusion/exclusion criteria. The papers were reviewed and graded for their quality, with a further 13 papers excluded.
A three-step qualitative analysis technique of metasynthesis was applied to the remaining 37 papers. Identification of similarities and differences enabled first-order interpretations to be identified, which were grouped into broader themes (second-order interpretations) by identifying concepts that applied to two or more studies. Further interpretation through synthesis of translation enabled third-order interpretations to emerge.

Findings
From the metasynthesis of the 37 papers, nine themes emerged: patient-centred care; benefits to the service; the need for knowledge; professional accountability and boundary setting; safety consciousness; barriers to effective prescribing; role preservation; power-shifts and inter-professional relationships; and culture of prescribing.
Molecular studies of Planetary Nebulae
Authors: Zhang Yong 
Published: August 2017

AbstractCircumstellar envelopes (CEs) around evolved stars are an active site for the production of molecules. After evolving through the Asymptotic Giant Branch (AGB), proto-planetary nebula (PPN), to planetary nebula (PN) phases, CEs ultimately merge with the interstellar medium (ISM). The study of molecules in PNe, therefore, is essential to understanding the transition from stellar to interstellar materials. So far, over 20 molecular species have been discovered in PNe. The molecular composition of PNe is rather different from those of AGB and PPNe, suggesting that the molecules synthesized in PN progenitors have been heavily processed by strong ultraviolet radiation from the central star. Intriguingly, fullerenes and complex organic compounds having aromatic and aliphatic structures can be rapidly formed and largely survive during the PPN/PN evolution. The similar molecular compositions in PNe and diffuse clouds as well as the detection of C60+ in the ISM reinforce the view that the mass-loss from PNe can significantly enrich the ISM with molecular species, some of which may be responsible for the diffuse interstellar bands. In this contribution, I briefly summarize some recent observations of molecules in PNe, with emphasis on their implications on circumstellar chemistry.
Understanding Galactic planetary nebulae with precise/reliable nebular abundances
Authors: García-Hernández D. A. , Ventura P. , Delgado-Inglada G. , Dell'Agli F. , Di Criscienzo M. , Yagüe A. 
Published: August 2017

AbstractWe compare recent precise/reliable nebular abundances - as derived from high-quality optical spectra and the most recent ICFs - in a sample of Galactic planetary nebulae (PNe) with nucleosynthesis predictions (HeCNOCl) from asymptotic giant branch (AGB) ATON models in the metallicity range Z⊙/4 < Z < 2Z⊙. According to the infrared dust features, the sample is divided among carbon-, oxygen-, and double-dust chemistry (CC, OC, and DC, respectively), providing an independent proxy for the nature of the PNe progenitors. Our AGB models, with diffusive overshooting from all the convective borders, nicely reproduce the O overabundances observed in CC PNe, indicating that they evolve from low-Z low-mass (∼1 −3 M⊙) AGB stars. This indicates that O is not always a good indicator of the original ISM metallicity and that the O production by low-mass stars should be considered in galactic-evolution models. The lowest metallicity OC PNe evolve from low-mass (∼1 M⊙) O-rich AGBs, while the higher metallicity ones (all with uncertain dust classifications) display a chemical pattern similar to the DC PNe. In agreement with the recent literature, the DC PNe mostly descend from high-mass (M > 3.5 M⊙) solar/supersolar metallicity AGBs that experience hot bottom burning (HBB), but other formation channels in low-mass AGBs like extra mixing, stellar rotation, binary interaction, or He pre-enrichment cannot be disregarded until more accurate C/O ratios can be obtained. Two DC PNe show the imprint of advanced CNO processing and deep second dredge-up, suggesting progenitors masses close to the limit to evolve as core collapse supernovae (above 6 M⊙). Their actual C/O ratios, if confirmed, indicate contamination from the third dredge-up, rejecting the hypothesis that the chemical composition of such high-metallicity massive AGBs is modified exclusively by HBB.
Photoionisation effects in hydrodynamical simulations of planetary nebulae
Authors: Hernández-Martínez L. , Estrella D. , Velázquez P. F. , Esquivel A. , Raga A. C. 
Published: August 2017

AbstractWe explored the photoionisation effects on both the proper motion and emission of planetary nebulae NGC 6302, by means of hydrodynamical simulations. We used the GUACHO code, which includes the photoionisation due to central source (Esquivel et al. 2009, Esquivel & Raga 2013). We model these PNe considering an interacting stellar fast wind with and ejected toroidally shaped slow wind (Uscanga et al. 2014). Synthetic Hα emission maps were obtained from our numerical results in order to do a comparison between the cases with and without photoionisation. Using a wavelets fittering method on our results for the ionisation case, we do not find an increase in the proper motion velocities, however we can see an accelerated expansion in both cases. For the ionisation case the Hα emission presents an increase.
Abundances and Gradients in M31 – A Chemical Study of Planetary Nebulae in the Substructures
Authors: Fang Xuan , García-Benito Rubén , Guerrero Martín A. , Liu Xiaowei , Zhang Yong , Yuan Haibo 
Published: August 2017

AbstractWe present deep optical spectroscopy of seven planetary nebulae (PNe) in the substructures of M31, three in the Northern Spur and four associated with the Giant Stream. The spectra were obtained with the OSIRIS spectrograph on the 10.4 m GTC. The detection of the [O iii] λ4363 auroral line in all PNe of our sample enables reliable abundance determinations. Our targets have low N/O (<0.5) and He/H ratios, indicating that they are probably Type II PNe. The PNe in our sample have rather homogeneous oxygen abundances, with an average value of 8.56±0.10. Based on the abundances as well as the spatial and kinematical information of our targets, we speculate that the Northern Spur and the Giant Stream might have the same origin. We raise a hypothesis that the dwarf satellite M32 might be responsible for these two substructures. New observations have recently been made to assess this hypothesis.
The halo of M49 and its environment as traced by planetary nebulae
Authors: Hartke Johanna , Arnaboldi Magda , Longobardi Alessia , Gerhard Ortwin , Freeman Ken , Okamura Sadanori 
Published: August 2017

AbstractWe investigate the stellar halo of the nearby elliptical Virgo-cluster galaxy M49 using Planetary Nebulae (PNe). M49 is the second-brightest galaxy of the Virgo cluster and is at the center of the Virgo subcluster B. We present an extended catalogue extracted from a narrow-band survey carried out with Subaru’s Suprime Cam, consisting of 735 PNe down to a limiting magnitude of m5007 = 29.3. This PNe population traces the halo out to 155 kpc from the galaxy’s center, which provides accurate measurement of the luminosity-specific PN-number (α-parameter) in the inner and outer regions of M49’s halo. We are also able to determine the morphological variation of the planetary nebulae luminosity function (PNLF), that may trace different parent stellar populations. This enables us to identify the transition from the PN-scarce, possibly metal-rich, galaxy halo to the PN-rich, metal-poor, outer component.
Herschel spectroscopic observations of PPNe and PNe
Authors: García-Lario Pedro , Ramos-Medina J. , Sánchez-Contreras C. 
Published: August 2017

AbstractWe are building a catalogue of interactively reprocessed observations of evolved stars observed with Herschel. The catalogue will offer not only the PACS and SPIRE spectroscopic data for each observation, but also complementary information from other infrared space observatories. As a first step, we are concentrating our efforts on two main activities: 1) the interactive data-reduction of more than 500 individual spectra obtained with PACS in the 55-210 μm range, available in the Herschel Science Archive; 2) the creation of a catalogue, accesible via a web-based interface and through the Virtual Observatory. Our ultimate goal is to carry out a comprehensive and systematic study of the far infrared properties of low-and intermediate-mass evolved stars using these data and enable science based on Herschel archival data. The objects cover the whole range of possible evolutionary stages in this short-lived phase of stellar evolution, from the AGB to the PN stage, displaying a wide variety of chemical and physical properties.
Expansion parallaxes and intrinsic stellar properties for 15 simple planetary nebulae
Authors: Schönberner Detlef , Jacob Ralf , Balick Bruce 
Published: August 2017

AbstractWe determined individual distances to a small number of rather round, quite regularly shaped planetary nebulae by combining their angular expansion in the plane of the sky with a spectroscopically measured expansion along the line of sight. For this goal, we combined up to three epochs of Hubble Space Telescope imaging data and determined the respective proper motions of rim and shell edges, and of other features as well. Ground-based radial velocities are assigned separately to the nebular rims and shells and used to determine individual distances, thereby assuming that the expansions in the line-of-sight and in the plane of sky are equal. We employed 1D radiation-hydrodynamics simulations of planetary nebulae evolution to correct for the difference between the spectroscopically measured expansion velocities of rim and shell and the expansion speeds of their respective shock fronts.
Central Stars of Planetary Nebulae
Authors: Jones David 
Published: August 2017

AbstractIn this brief invited review, I will attempt to summarise some of the key areas of interest in the study of central stars of planetary nebulae which (probably) will not be covered by other speakers’ proceedings. The main focus will, inevitably, be on the subject of multiplicity, with special emphasis on recent results regarding triple central star systems as well as wide binaries which avoid a common-envelope phase. Furthermore, in light of the upcoming release of Kepler’s Campaign 11 data, I will discuss a few of the prospects from that data including the unique possibility to detect merger products.
Spitzer IRS spectroscopy of planetary nebulae
Authors: Ramos-Larios G. , Guerrero M. A. , Mata H. , Fang X. , Nigoche-Netro A. , Toalá J. A. , Rubio G. 
Published: August 2017

AbstractWe present Spitzer Space Telescope archival mid-infrared (mid-IR) spectroscopy of a sample of eleven planetary nebulae (PNe). The observations, acquired with the Spitzer Infrared Spectrograph (IRS), cover the spectral range 5.2-14.5 μm that includes the H2 0-0 S(2) to S(7) rotational emission lines. This wavelength coverage has allowed us to derive the Boltzmann distribution and calculate the H2 rotational excitation temperature (Tex). The derived excitation temperatures have consistent values ≃ 900 ±70 K for different sources despite their different structural components. We also report the detection of mid-IR ionic lines of [Ar iii], [S iv], and [Ne ii] in most objects, and polycyclic aromatic hydrocarbon (PAH) features in a few cases.
Post-AGB nebular studies
Authors: Lagadec Eric 
Published: August 2017

AbstractThis review presents the latest advances in the nebular studies of post-AGB objects. Post-AGB stars are great tools to test nucleosynthesis and evolution models for stars of low and intermediate masses, and the evolution of dust in harsh environment. I will present the newly discovered class of post-RGB stars, formed via binary interaction on the RGB. Binary systems can also lead to the formation of two class of aspherical post-AGB, the Proto-Planetary Nebulae and the naked post-AGBs (dusty RV Taus, a.k.a. Van Winckel’s stars).
X-ray Studies of Planetary Nebulae
Authors: Montez Rodolfo 
Published: August 2017

AbstractX-ray emission from planetary nebulae (PNe) provides unique insight on the formation and evolution of PNe. Past observations and the ongoing Chandra Planetary Nebulae Survey (ChanPlaNS) provide a consensus on the two types of X-ray emission detected from PNe: extended and compact point-like sources. Extended X-ray emission arises from a shocked “hot bubble” plasma that resides within the nebular shell. Cooler than expected hot bubble plasma temperatures spurred a number of potential solutions with one emerging as the likely dominate process. The origin of X-ray emission from compact sources at the location of the central star is less clear. These sources might arise from one or combinations of the following processes: self-shocking stellar winds, spun-up binary companions, and/or accretion, perhaps from mass transfer, PN fallback, or debris disks. In the discovery phase, X-ray studies of PNe have mainly focused on the origin of the various emission processes. New directions incorporate multi-wavelength observations to study the influence of X-ray emission on the rest of the electromagnetic spectrum.
Progress and Application of The Initial-Final Mass Relation
Authors: Cummings Jeffrey D. 
Published: August 2017

AbstractThe stellar life cycle is dominated by phases such as the hydrogen-burning stage and the remnant white dwarf cooling phase. However, between these two stages, stars dramatically transform themselves by losing the bulk of their mass. Planetary nebulae (PNe) provide a powerful clue to the processes involved in this transformation, but they are very complex. Over the past 15 years, a new wave of imaging and spectroscopy programs have uncovered the remnants of PNe, white dwarfs, in a wide range of well-measured environments. With this we can map the masses and temperatures of the stellar remnants to the properties of their progenitors. This work has now led to the first uniform mapping of the initial-final mass relation from 1.5 to 7 M⊙. The resulting relation is a fundamental input to our understanding of stellar evolution for low and intermediate-mass stars that produce PNe and has a wide range of applications.
Resolving the Disk-Halo Degeneracy using Planetary Nebulae
Authors: Aniyan S. , Freeman K. C. , Arnaboldi M. , Gerhard O. , Coccato L. , Fabricius M. , Kuijken K. , Merrifield M. 
Published: August 2017

AbstractThe decomposition of the 21 cm rotation curve of galaxies into contribution from the disk and dark halo depends on the adopted mass to light ratio (M/L) of the disk. Given the vertical velocity dispersion (σz) of stars in the disk and its scale height (hz), the disk surface density and hence the M/L can be estimated. Earlier works have used this technique to conclude that galaxy disks are submaximal. Here we address an important conceptual problem: star-forming spirals have an old (kinematically hot) disk population and a young cold disk population. Both of these populations contribute to the integrated light spectra from which σz is measured. The measured scale height hz is for the old disk population. In the Jeans equation, σz and hz must pertain to the same population. We have developed techniques to extract the velocity dispersion of the old disk from integrated light spectra and from samples of planetary nebulae. We present the analysis of the disk kinematics of the galaxy NGC 628 using IFU data in the inner regions and planetary nebulae as tracers in the outer regions of the disk. We demonstrate that using the scale height of the old thin disk with the vertical velocity dispersion of the same population, traced by PNe, results in a maximal disk for NGC 628. Our analysis concludes that previous studies underestimate the disk surface mass density by ~ 2, sufficient to make a maximal disk for NGC 628 appear like a submaximal disk.
GTC/CanariCam mid-IR imaging of the fullerene-rich planetary nebula IC 418
Authors: Díaz-Luis J. J. , García-Hernández D. A. , Manchado A. , García-Lario P. , Villaver E. , García-Segura G. 
Published: August 2017

AbstractThe formation process(es) of fullerenes in space is still uncertain and several mechanisms have been proposed in the literature. In particular, the most accepted idea to explain the simultaneous presence of fullerenes and PAH-like emission in the H-rich circumstellar envelopes of PNe is that these molecular species may be formed from the photochemical processing of a carbonaceous compound with a mixture of aromatic and aliphatic structures, which should be a major constituent of their circumstellar envelopes. Here we present seeing-limited narrow-band mid-IR GTC/CanariCam images of the fullerene-containing PN IC 418. The narrow-band images cover the 9−13, 11.3, and 17.4 μm emission features (and their adjacent continua) in this extended PN. We study the relative sub-arcsecond spatial distribution of the nebula in these filters with the intention of getting some clues about the formation process of fullerenes in H-rich circumstellar environments.
Mid-Infrared Studies of the Cool Dust Distribution in Bipolar Planetary Nebulae
Authors: Asano Kentaro , Miyata Takashi , Kamizuka Takafumi , Ueta Toshiya 
Published: August 2017

AbstractTo understand mass loss history and mass loss and dust formation history of massive AGB stars, we carried out observations of three bipolar planetary nebulae (BPNe) in 30 micron bands from a ground-based telescope. All of our targets have a compact strong emission source in the mid-infrared (MIR) around the position of the central star of planetary nebula (CSPN). These detected emissions can be originated from cool dust. Our results show that the cool dust component is compactly distributed and much more massive than previous studies indicated. These findings suggest that they experienced a strong mass loss into the equatorial direction in past.
The systematic uncertainties introduced by atomic data in nebular abundance determinations
Authors: de Dios Leticia Juan , Rodríguez Mónica 
Published: August 2017

AbstractAtomic data selection is one important source of systematic uncertainty since there are important variations between the values provided by different authors. We explore the effect of using different atomic data in the determination of physical conditions and chemical abundances in a sample of Galactic planetary nebulae and Hii regions. We find that the available datasets introduce significant differences in the results, especially at densities above 104 cm−3, where O/H and N/O reach uncertainties higher than a factor of 4.
The VIRGO PN population and the mass assembly in M87
Authors: Longobardi Alessia , Arnaboldi Magda , Gerhard Ortwin 
Published: August 2017

AbstractCosmological simulations allow us to study in detail the evolution of galaxy halos in cluster environments, but the extremely low surface brightness of such components makes it difficult to gather observational constraints. Planetary nebulas (PNs) offer a unique tool to investigate these environments owing to their strong [OIII] emission line. We study the light and kinematics of the Virgo cluster and its central galaxy, M87, prime targets to address the topic of galaxy formation and evolution in dense environments. We make use of a deep and extended PN sample (~300 objects) that extends out to 150 kpc in radius from M87’s centre. We show that at all distance the galaxy halo overlaps with the Virgo intracluster light (ICL). Halo and ICL are dynamically distinct components with different parent stellar populations, consistent with the halo of M87 being redder and more metal rich than the ICL. The synergy between PN kinematic information and deep V/B-band photometry made it possible to unravel an ongoing accretion process in the outskirt of M87. This accretion event represents a non-negligible perturbation of the halo light, showing that this galaxy is still growing by accretion of smaller systems.
Shaping planetary nebulae with jets in inclined triple stellar systems
Authors: Akashi Muhammad , Soker Noam 
Published: August 2017

AbstractWe conduct three-dimensional hydrodynamical simulations of two opposite jets launched obliquely to the orbital plane around an asymptotic giant branch (AGB) star and within its dense wind, and demonstrate the formation of a ‘messy’ planetary nebula (PN), namely, a PN lacking any type of symmetry (highly irregular). In building the initial conditions we assume that a tight binary system orbits the AGB star, and that the orbital plane of the tight binary system is inclined to the orbital plane of binary system and the AGB star. We further assume that the accreted mass onto the tight binary system forms an accretion disk around one of the stars, and that the plane of the disk is in between the two orbital planes. The highly asymmetrical lobes that we obtain support the notion that messy PNe might be shaped by triple stellar systems.
Circumstellar spirals/shells/arcs: the message from binary stars
Authors: Kim Hyosun 
Published: August 2017

AbstractA consensus has grown in the past few decades that binarity is key to understanding the morphological diversities of the circumstellar envelopes (CSEs) surrounding stars in the Asymptotic Giant Branch (AGB) to Planetary Nebula (PN) phase. The possible roles of binaries in their shaping have, however, yet to be confirmed. Meanwhile, recurrent patterns are often found in the CSEs of AGB stars and the outer halos of PNe, providing a fossil record of the mass loss during the AGB phase. In this regard, recent molecular line observations using interferometric facilities have revealed the spatio-kinematics of such patterns. Numerical simulations of binary interactions producing spiral-shells have been extensively developed, revealing new probes for extracting the stellar and orbital properties from these patterns. I review recent theoretical and observational investigations on the circumstellar spiral-shell patterns and discuss their implications in linking binary properties to the asymmetric ejection events in the post-AGB phase.
A New Model of NGC 6210 to Solve its Abundance Discrepancy Problem
Authors: Escalante V. , Toalá J. A. 
Published: August 2017

AbstractWe present a model that solves the abundance discrepancy problem for NGC 6210. The model proposes a high abundance of CNONe elements that lowers the temperature of the central parts of the nebula. The colder gas model reproduces the observed intensity of the strong [N ii] and [O iii] emission lines, and increases the predicted weak recombination lines towards their observed values. We examine how the usual nebular diagnostic line ratios depend on model abundances.