bluuebunny/crossref_metadata_2025_split huggingface dataset:
Trajectories of caregiver burden in families of adult cystic fibrosis patients
Authors: Wojtaszczyk Ann , Glajchen Myra , Portenoy Russell K. , Berdella Maria , Walker Patricia , Barrett Malcolm , Chen Jack , Plachta Amy , Balzano Julie , Fresenius Ashley , Wilder Kenya , Langfelder-Schwind Elinor , Dhingra Lara 
Published: October 2017

ABSTRACTObjectives:Little is known about the experience of family caregivers of adults with cystic fibrosis (CF). This information is important for the identification of caregivers at risk for burden.Methods:This was a longitudinal analysis of survey data obtained from caregivers of adult CF patients participating in an early intervention palliative care trial. Caregivers completed the validated Brief Assessment Scale for Caregivers (BASC) repeatedly over a 28-month period. Mixed-effects modeling evaluated multivariate associations with positive and negative caregiver perceptions over time.Results:Of the 54 caregivers, 47.9% were spouses. The mean age was 50.9 years (SD = 13.2); 72.2% were women; 75.9% were married; and 63.0% were employed. At baseline, the BASC revealed large variations in positive and negative perceptions of caregiving. Although average scores over time were unchanging, variation was greater across caregivers than within caregivers (0.49 vs. 0.27, respectively). At baseline, the positive impact of caregiving in the sample was higher than the negative impact. Multivariate analysis revealed that patients' baseline pulmonary function and their full-time employment status predicted caregiver burden over time.Significance of results:Caregivers of CF patients varied in their positive and negative caregiving experiences, although burden levels in individual caregivers were stable over time. When the disease was advanced, caregivers of CF patients experienced more overall burden but also more positive impact. This suggests that the role of caregivers may become more meaningful as disease severity worsens. In addition, full-time patient employment was associated with lower caregiver burden regardless of disease severity. This suggests that burden in CF caregivers may be predicted by financial strain or benefits conferred by patient employment. These associations require further investigation to determine whether highly burdened caregivers can be identified and assisted using tailored interventions.
Prevalence of common honey bee pathogens at selected apiaries in Kenya, 2013/2014
Authors: Ongus Juliette R. , Fombong Ayuka T. , Irungu Janet , Masiga Daniel , Raina Suresh 
Published: October 2017

AbstractThe present study was part of a larger surveillance effort to identify the determinants of African honey bee health, and, particularly, to detect honey bee pathogens across Kenya, where 160 colonies were examined from 32 apiaries (five colonies/apiary). From each colony, 20 individual foragers, nurse bees, worker pupae, and drone pupae were sampled separately. These were organized as 30 foragers, 32 nurse bees, 28 worker pupae, and 10 drone pupae pools. Nucleic acid was extracted from the pooled homogenates and tested using a panel of 18 different (RT-)PCR methods targeted at detectingPaenibacillus larvae,Melissococcus plutonius,Ascophaera apis,Aspergillusspp.,Nosema ceranae, N. apis,Deformed wing virus(DWV),Varroa destructor virus 1(VDV 1),Acute bee paralysis virus(ABPV),Sacbrood virus(SBV),Israeli acute paralysis virus(IAPV),Black queen cell virus(BQCV),Chronic bee paralysis virus(CBPV), andKashmir bee virus. All amplified bands were sequenced and compared to the GenBank database. VDV 1 was the most abundant virus at 50% prevalence in the 100 bee pools. It was closely followed by DWV at 44%. The others were BQCV (36%), SBV (14%), IAPV (9%), ABPV (8%), andN. ceranae(5%). The pathogens co-existed within apiaries. VDV 1 was present in 66% of the apiaries, DWV in 69%, BQCV in 69%, SBV in 28%, IAPV in 22%, ABPV in 19%, andN. ceranaein 13%. The study concludes that these pathogens should be incorporated in honey bee disease surveillance activities in the region.
Detecting Thermal X-Ray Emission and Proper Motions in RX J1713.7-3946
Authors: Katsuda Satoru , Acero Fabio , Tominaga Nozomu , Ballet Jean , Fukui Yasuo , Hiraga Junko S. , Koyama Katsuji , Lee Shiu-Hang , Mori Koji , Nagataki Shigehiro , Ohira Yutaka , Petre Robert , Sano Hidetoshi , Takeuchi Yoko , Tamagawa Toru , Tsuji Naomi , Tsunemi Hiroshi , Uchiyama Yasunobu 
Published: October 2017

AbstractWe report detections of thermal X-ray line emission and proper motions in the supernova remnant (SNR) RX J1713.7-3946, the prototype of the small class of synchrotron dominated SNRs. Based on deep XMM-Newton observations, we find clear line features including Ne Lyα, Mg Heα, and Si Heα from the central portion of the remnant. The metal abundance ratios suggest that the thermal emission originates from core-collapse SN ejecta arising from a relatively low-mass (≲20 M⊙) progenitor. In addition, using XMM-Newton observations on a 13 yr time interval, we have measured expansion in the southeastern rim to be ~0.75″ yr−1 or ~3500 km s−1 at a distance of 1 kpc. Given this, we derive an upstream density to be ~0.01 cm−3, compatible with the lack of thermal X-rays from the shocked ambient medium. We also estimate the age of the remnant to be ~1200–1600 yr, roughly consistent with the idea that RX J1713.7-3946 is the remnant of SN 393.
Multimessenger Predictions from 3D General-Relativistic Core-Collapse Supernovae Models
Authors: Kotake Kei , Kuroda Takami , Hayama Kazuhiro 
Published: October 2017

AbstractIn this contribution, we present results from fully general-relativistic three-dimensional (3D) simulations of a non-rotating 15M⊙ star using different nuclear equations of state (EOSs). We show that the SASI (standing-accretion-shock-instability) activity occurs much more vigorously in models with softer EOS. By performing detailed analysis of the gravitational-wave (GW) emission, we find a new GW signature that is produced predominantly by the SASI-induced downflows to the proto-neutron star. We discuss the detectability of the GW signal by performing a coherent network analysis where multiple detectors including LIGO Hanford, LIGO Livingston, VIRGO, and KAGRA are considered. We point out that the GW signal, whose typical frequency is in the best sensitivity range of the laser-interferometers, could potentially provide the live broadcast that pictures how the supernova shock is dancing in the core. The detection horizon of the signal is estimated as 2~3 kpc for the current generation detectors, which can extend up to ~100 kpc for the third generation detectors like Cosmic Explorer. We furthermore perform a correlation analysis between the SASI-modulated GW and neutrino signals. Our results show that the time correlation of the two signals becomes highest when we take into account the travel timescale of adverting material from the (average) neutrino-sphere to the proto-neutron star surface.
Magnetically assisted explosions of weakly magnetized stars
Authors: Sawai Hidetomo , Yamada Shoichi 
Published: October 2017

AbstractWe carried out high resolution simulations of weakly-magnetized core-collapse supernovae in two-dimensional axisymmetry in order to see the influence of the magnetic field and rotation on the explosion. We found that the magnetic field amplified by magnetorotational instability (MRI) has a great positive impact on the explosion by enhancing the neutrino heating, provided that the progenitor has large angular momentum close to the highest value found in stellar evolution calculations. We also found that even for progenitors neither involving strong magnetic flux nor large angular momentum, the magnetic field is greatly amplified by the convection aand rotation, and this leads to the boost of the explosion again by enhancing the neutrino heating.
Supernova 1986J: a Neutron Star or Black Hole in the Centre?
Authors: Bietenholz Michael F. 
Published: October 2017

AbstractSupernova 1986J is almost the same age as SN 1987A, but was Type IIn, and likely had a massive progenitor. Located at 10 Mpc in NGC 891, it is one of the few supernovae whose radio emission can be resolved using VLBI. We present a new 5-GHz global-VLBI image of SN 1986J from 2014 as well as broadband VLA flux-density measurements. SN 1986J is unusual in that a compact synchrotron radio-emitting component appeared in the centre of the expanding shell of ejecta ~14 yr after the explosion, which now dominates the VLBI image. The central component is stationary to within the uncertainties (<570 km s−1), and it has a marginally resolved HWHM radius of (6.7−3.7+0.7) × 1016cm. The shell has expanded with averagev≃ 5400 km s−1. The central component’s 5-GHz flux density is still increasing with time, and at present it has a 5-GHz νLνluminosity of ~4 × 1035erg s−1, ~20 times that of the Crab Nebula. The central component may be due to a newly formed pulsar wind nebula, or an accreting black hole, or it may be due to interaction of the supernova shock with a highly structured environment left over from a progenitor which was in a close binary system. We discuss the newest observations and the constraints on its nature.
Spatial distribution of radionuclides in 3D models of SN 1987A and Cas A
Authors: Janka Hans-Thomas , Gabler Michael , Wongwathanarat Annop 
Published: October 2017

AbstractFostered by the possibilities of multi-dimensional computational modeling, in particular the advent of three-dimensional (3D) simulations, our understanding of the neutrino-driven explosion mechanism of core-collapse supernovae (SNe) has experienced remarkable progress over the past decade. First self-consistent, first-principle models have shown successful explosions in 3D, and even failed cases may be cured by moderate changes of the microphysics inside the neutron star (NS), better grid resolution, or more detailed progenitor conditions at the onset of core collapse, in particular large-scale perturbations in the convective Si and O burning shells. 3D simulations have also achieved to follow neutrino-driven explosions continuously from the initiation of the blast wave, through the shock breakout from the progenitor surface, into the radioactively powered evolution of the SN, and towards the free expansion phase of the emerging remnant. Here we present results from such simulations, which form the basis for direct comparisons with observations of SNe and SN remnants in order to derive constraints on the still disputed explosion mechanism. It is shown that predictions based on hydrodynamic instabilities and mixing processes associated with neutrino-driven explosions yield good agreement with measured NS kicks, light-curve properties of SN 1987A and asymmetries of iron and 44Ti distributions observed in SN 1987A and Cassiopeia A.
Balmer-dominated shocks in Tycho’s SNR: omnipresence of CRs
Authors: Knežević Sladjana , Läsker Ronald , van de Ven Glenn , Font Joan , Raymond John C. , Bailer-Jones Coryn A. L. , Beckman John , Morlino Giovanni , Ghavamian Parviz , Hughes John P. , Heng Kevin 
Published: October 2017

AbstractWe present wide-field, spatially and highly resolved spectroscopic observations of Balmer filaments in the northeastern rim of Tycho’s supernova remnant in order to investigate the signal of cosmic-ray (CR) acceleration. The spectra of Balmer-dominated shocks (BDSs) have characteristic narrow (FWHM ~ 10 km s−1) and broad (FWHM ~ 1000 km s−1) Hα components. CRs affect the Hα-line parameters: heating the cold neutrals in the interstellar medium results in broadening of the narrow Hα-line width beyond 20 km s−1, but also in reduction of the broad Hα-line width due to energy being removed from the protons in the post-shock region. For the first time we show that the width of the narrow Hα line, much larger than 20 km s−1, is not a resolution or geometric effect nor a spurious result of a neglected intermediate (FWHM ~ 100 km s−1) component resulting from hydrogen atoms undergoing charge exchange with warm protons in the broad-neutral precursor. Moreover, we show that a narrow line width ≫ 20 km s−1extends across the entire NE rim, implying CR acceleration is ubiquitous, and making it possible to relate its strength to locally varying shock conditions. Finally, we find several locations along the rim, where spectra are significantly better explained (based on Bayesian evidence) by inclusion of the intermediate component, with a width of 180 km s−1on average.
Synergy SKA - CTA: Supernova remnants as cosmic accelerators
Authors: Ingallinera Adriano , Trigilio Corrado , Umana Grazia , Leto Paolo , Buemi Carla , Schillirò Francesco , Bufano Filomena , Riggi Simone , Cavallaro Francesco 
Published: October 2017

AbstractSupernova remnants (SNRs) are one of the most important sites where particles are accelerated with high efficiency and in a wide range of energies, becoming an important component of cosmic rays. A good test for this hypothesis will be possible using the data collected by next-generation radio and gamma-ray observatories, like the Square Kilometre Array (SKA) and the Cherenkov Telescope Array (CTA). Radio emission is fundamental to explore the SNR environment and to shed light on the physical processes involved in particle acceleration, providing direct links to high-energy physics. Two cases of SNRs recently studied in radio are presented, showing the importance of high-resolution radio images. An overview of SKA and its precursors is given with our ongoing preparation work. In particular, we present the EMU survey and the pathfinder project SCORPIO. Finally a direct view of the tight connection between SKA and CTA future studies of SNRs is provided.
X-raying the evolution of SN 1987A
Authors: Kashyap Vinay L. , van Dyk David , McKeough Katy , Primini Frank , Jerius Diab , Gowrishankar Akshay , Siemiginowska Aneta , Zezas Andreas 
Published: October 2017

AbstractSN 1987A has been observed with the Chandra X-ray Observatory over the entire course of the mission. We have re-analyzed the archival data by constructing an empirical point spread function and reconstructing high-resolution images using a Bayesian multi-scale image reconstruction algorithm. We are able to resolve structure in the equatorial ring of SN 1987A with unprecedented detail, at scales of $\approx \frac{1}{4}$ arcsec. We describe how the point spread function is constructed, and the reconstruction method, and explore the evolution of the inner ring at different epochs and passbands.
The infancy of supernova remnants: evolving a supernova into its remnant in 3D
Authors: Gabler Michael , Janka Hans-Thomas , Wongwathanarat Annop 
Published: October 2017

AbstractRecently, first neutrino-driven supernova explosions have been obtained in 3D, self-consistent, first-principle simulations, these models are still not always exploding robustly and, in general, the explosions are not sufficiently energetic. To constrain the explosion mechanism, and the related uncertainties, it is thus very helpful to consider observational constraints: pulsar kicks, progenitor association and supernova remnants (SNR). Recent observations of asymmetries in the supernova ejecta of Cas A are very promising, to compare to long-term simulations of the explosion. In addition 3D observations of SN87A are becoming more constraining on the geometry of the ejected material during the explosion. In this talk I will discuss our efforts to model the late time evolution of a 3D supernova explosion, where we include the effects of beta decay, which inflates the structures rich in 56Ni. The structures we find in the simulations depend on the quantities plotted.
Supernova Remnant-Cosmic Ray connection: a modern view
Authors: Morlino Giovanni 
Published: October 2017

AbstractThe Cosmic Ray (CR) physics has entered a new era driven by high precision measurements coming from direct detection (especially AMS-02 and PAMELA) and also from gamma-ray observations (Fermi-LAT). In this review we focus our attention on how such data impact the understanding of the supernova remnant paradigm for the origin of CRs. In particular we discuss advancement in the field concerning the three main stages of the CR life: the acceleration process, the escape from the sources and the propagation throughout the Galaxy. We show how the new data reveal a phenomenology richest than previously thought that could even challenge the current understanding of CR origin.
Evidence for a wide electron spectra scatter among different SNR regions from high radio-frequency observations
Authors: Pellizzoni A. , Egron E. , Iacolina M. N. , Loru S. , Marongiu M. , Righini S. , Cardillo M. , Giuliani A. , Mulas S. , Murtas G. , Simeone D. 
Published: October 2017

AbstractIn the framework of the Sardinia Radio Telescope (SRT) Early Science Program, we obtained single-dish high-resolution imaging of the Supernova Remnants IC443 and W44 at 7 GHz. By coupling them with SRT 1.5 GHz maps, we provided spatially-resolved spectral measurements that are highlighting a spread in spectral slope distribution. The observed features range from flat or slightly inverted spectra corresponding to bright radio limbs and filaments, to relatively steep spectra in fainter radio regions. Different theoretical possibilities explaining the above challenging findings are discussed. In particular, we exclude that the observed region-dependent wide spread in spectral slope distribution could be related to absorption processes. Our high-frequency results can be directly related to distinct electron populations in the SNRs including secondary hadronic electrons and resulting from different shocks conditions and/or undergoing different cooling processes. Integrated fluxes associated with the whole SNRs obtained by SRT in comparison with previous results in the literature support the evidence for a slight spectral steepening above 1 GHz for both sources, which could be related to primary electrons or more likely secondary hadronic electrons cut-offs.
Disentangling hadronic from leptonic emission in the composite SNR G326.3-1.8
Authors: Devin Justine , Acero Fabio , Ballet Jean 
Published: October 2017

AbstractG326.3-1.8 (also known as MSH 15-56) has been detected in radio as a middle-aged composite supernova remnant (SNR) consisting of a SNR shell and a pulsar wind nebula (PWN) which has been crushed by the reverse shock. With the recent Fermi-LAT data release Pass 8 providing increased acceptance and angular resolution, we investigate the morphology of this SNR to disentangle the PWN from the SNR contributions and understand the nature of the γ-ray emission. We thus perform a morphological and spectral analysis from 300 MeV to 300 GeV which highlights the contributions from these two components. The simplest interpretation is hadronic emission from the SNR and harder leptonic emission from the PWN.
The diversity of GRBs and their SNe: Observations from the 10.4m GTC
Authors: de Ugarte Postigo Antonio , Thöne Christina , Cano Zach , Kann David Alexander , Izzo Luca , Ramírez Rubén Sánchez , Bensch Katarzyna , Sagues Ana 
Published: October 2017

AbstractObserving the supernovae (SNe) associated to the different types of gamma-ray bursts (GRBs) is one of the few means to study their progenitors. In the past years, it has become clear that GRB-like events are more heterogeneous than previously thought. There is a marked difference between long GRBs, which are produced by the collapse of very massive stars and are normally associated with broad-lined type Ic SNe, and short bursts, which occur when two compact objects merge and that, at least in some cases, can produce an associated kilonova. Moreover, the SNe associated with different sub-types of long GRBs are also seen to differ, especially those associated with ultra-long duration GRBs. To address this issue in a systematic way we started an observing programme in 2010 at the 10.4m GTC telescope. Here we present some results of our programme, including the detection of 12 new GRB-SNe. Highlights of our sample are the discovery of the first spectroscopic SN associated with a highly energetic (Eγ, iso ~ 1054 erg) “cosmological” burst (GRB 130427A), the study of the SN associated with a shock-breakout GRB (GRB 140606B) and the SN associated with the peculiar ultra-long GRB 101225A at z = 0.85. The sample includes also the follow-up of several short GRBs in search for kilonovae emission (GRB 130603B and GRB 160821B are important examples). Amongst our latest results we present the photometric and spectroscopic observations of the SNe associated with GRB 150818A and GRB 161219B.
Progenitors of Core-Collapse Supernovae
Authors: Hirschi R. , Arnett D. , Cristini A. , Georgy C. , Meakin C. , Walkington I. 
Published: October 2017

AbstractMassive stars have a strong impact on their surroundings, in particular when they produce a core-collapse supernova at the end of their evolution. In these proceedings, we review the general evolution of massive stars and their properties at collapse as well as the transition between massive and intermediate-mass stars. We also summarise the effects of metallicity and rotation. We then discuss some of the major uncertainties in the modelling of massive stars, with a particular emphasis on the treatment of convection in 1D stellar evolution codes. Finally, we present new 3D hydrodynamic simulations of convection in carbon burning and list key points to take from 3D hydrodynamic studies for the development of new prescriptions for convective boundary mixing in 1D stellar evolution codes.
High-resolution spectral imaging of SNR W44 and IC443 at 22 GHz with the Sardinia Radio Telescope
Authors: Loru S. , Pellizzoni A. , Egron E. , Iacolina N. , Righini S. , Marongiu M. , Mulas S. , Murtas G. , Simeone D. , Pilia M. , Bachetti M. , Trois A. , Ricci R. , Melis A. , Concu R. 
Published: October 2017

AbstractIn the framework of the Astronomical Validation and Early Science activities of the Sardinia Radio Telescope (SRT, www.srt.inaf.it), we performed 22 GHz imaging observations of SNR W44 and IC443. Thanks to the single-dish imaging performances of SRT and innovative ad hoc imaging techniques, we obtained maps that provide a detailed view of the structure of the remnants. We are planning to exploit the high-frequency radio data of SNRs to better characterize the spatially-resolved spectra and search for possible spectral steepening or breaks in selected SNR regions, assessing the high-energy tail of the region-dependent electron distribution.
Go Pro Bono
Authors: Pietraszkiewicz Agnieszka , Soppe Birthe , Formanowicz Magdalena 
Published: October 2017

Abstract. Crowdfunding enables fundraising of various ventures by collecting money from several donors. We argue that the inclusion of prosocial language contributes to success in this new domain of resource acquisition. In Study 1, we analyzed 164,056 projects from the online crowdfunding platform Kickstarter and found that the higher the percentage of prosocial words employed in a project’s description, the larger the number of investors and the greater the chances of reaching a funding goal. In Study 2 (N = 234), an experimental study, we documented that the use of prosocial words increases the support people thought they would give to a project. Our results indicate that people want to invest their financial resources in ventures that contribute to prosocial goals.