bluuebunny/crossref_metadata_2025_split huggingface dataset:
Was Montesquieu a Liberal Republican?
Authors: de Dijn Annelien 
Published: January 2014

AbstractThis paper sets out to criticize Thomas Pangle's and Paul Rahe's reading ofThe Spirit of the Lawsas a contribution to liberal republicanism, arguing instead that Montesquieu's text is better understood as a defense of liberal monarchism. Pangle's and Rahe's interpretation ofThe Spirit of the Lawsas an unequivocal defense of the English modern republic is wrongheaded. Montesquieu in fact spent much more of his time and energy outlining another and very different political model, moderate monarchy, embodied not by England but by the government under which he lived—France. This conclusion has profound implications for our understanding not just ofThe Spirit of the Lawsbut also of the history of early modern political thought more generally speaking, showing that the political debate of this period cannot be reduced to a struggle between classical and modern republicans.
Learning from Franklin's Mistakes: Self-Interest Rightly Understood in theAutobiography
Authors: McClure Christopher S. 
Published: January 2014

AbstractBenjamin Franklin divides the mistakes he lists in theAutobiographyinto “errata” and “great errata.” He derived no benefit from the latter, but some benefit from the former. Examining Franklin's regret, or lack of regret, at these errata opens a window onto Franklin's understanding of morality. The laxity in his list of virtues and his flexibility with regard to conventional morals stem from the insight Franklin tells us he gained from these errata. For Franklin, or at least his persona in theAutobiography, there was no conflict between egoism and altruism, and he is therefore the embodiment of a type of self-interest well understood. Tracing the story of the errata, which Franklin inserted into an earlier draft of the work's first part, and Franklin's later actions provides the key to understanding the rhetorical strategy of theAutobiography, and the reason he never wrote his proposedArt of Virtue.
Can tasks be inherently boring?
Authors: Charney Evan 
Published: January 2014

AbstractKurzban et al. argue that the experiences of “effort,” “boredom,” and “fatigue” are indications that the costs of a task outweigh its benefits. Reducing the costs of tasks to “opportunity costs” has the effect of rendering tasks costless and of denying that they can be inherently boring or tedious, something that “vigilance tasks” were intentionally designed to be.
USING PREDICTION INTERVALS FROM RANDOM-EFFECTS META-ANALYSES IN AN ECONOMIC MODEL
Authors: Teljeur Conor , O'Neill Michelle , Moran Patrick , Murphy Linda , Harrington Patricia , Ryan Máirín , Flattery Martin 
Published: January 2014

Objectives: When incorporating treatment effect estimates derived from a random-effect meta-analysis it is tempting to use the confidence bounds to determine the potential range of treatment effect. However, prediction intervals reflect the potential effect of a technology rather than the more narrowly defined average treatment effect. Using a case study of robot-assisted radical prostatectomy, this study investigates the impact on a cost-utility analysis of using clinical effectiveness derived from random-effects meta-analyses presented as confidence bounds and prediction intervals, respectively.Methods: To determine the cost-utility of robot-assisted prostatectomy, an economic model was developed. The clinical effectiveness of robot-assisted surgery compared with open and conventional laparoscopic surgery was estimated using meta-analysis of peer-reviewed publications. Assuming treatment effect would vary across studies due to both sampling variability and differences between surgical teams, random-effects meta-analysis was used to pool effect estimates.Results: Using the confidence bounds approach the mean and median ICER was €24,193 and €26,731/QALY (95%CI: €13,752 to €68,861/QALY), respectively. The prediction interval approach produced an equivalent mean and median ICER of €26,920 and €26,643/QALY (95%CI: -€135,244 to €239,166/QALY), respectively. Using prediction intervals, there is a probability of 0.042 that robot-assisted surgery will result in a net reduction in QALYs.Conclusions: Using prediction intervals rather than confidence bounds does not affect the point estimate of the treatment effect. In meta-analyses with significant heterogeneity, the use of prediction intervals will produce wider ranges of treatment effect, and hence result in greater uncertainty, but a better reflection of the effect of the technology.
Recent Hubble Space Telescope Observations of SN 1987A: Broad Emission Lines
Authors: France Kevin 
Published: January 2014

AbstractObservations with the Hubble Space Telescope (HST), conducted since 1990, have allowed us to create a “movie” of the evolution of the core-collapse supernova SN 1987A from 3–25 years after the explosion. Critical to understanding the late time evolution of SN 1987A was the successful HST Servicing Mission 4 in May 2009. The repair of the STIS instrument and the installation of the WFC3 imager and COS spectrograph have provided crucial data points for understanding the temporal variability in the physical structure and energy sources for SN 1987A, as well as measurements of the chemical abundances of the ejecta. In this proceeding, I will focus on two topics that have made use of the expanded capability of HST and highlight the importance of access to a UV/optical space observatory for the studies of local supernovae: 1) 2) The decreasing maximum velocity of neutral hydrogen crossing the reverse shock front and the role of soft X-ray/EUV heating in the outer supernova debris and 2) The detection of metals (N4+ and C3+ ions) crossing the reverse shock front and CNO processing in the progenitor star.
Radio Observations of Supernova 1987A
Authors: Staveley-Smith L. , Potter T. M. , Zanardo G. , Gaensler B. M. , Ng C.-Y. 
Published: January 2014

AbstractSupernovae and their remnants are believed to be prodigious sources of Galactic cosmic rays and interstellar dust. Understanding the mechanisms behind their surprisingly high production rate is helped by the study of nearby young supernova remnants. There has been none better in modern times than SN1987A, for which radio observations have been made for over a quarter of a century. We review extensive observations made with the Australia Telescope Compact Array (ATCA) at centimetre wavelengths. Emission at frequencies from 1 to 100 GHz is dominated by synchrotron radiation from an outer shock front which has been growing exponentially in strength from day 3000, and is currently sweeping around the circumstellar ring at about 4000 km s−1. Three dimensional models of the propagation of the shock into the circumstellar medium are able to reproduce the main observational features of the remnant, and their evolution. We find that up to 4% of the electrons encountered by the shock are accelerated to relativistic energies. High-frequency ALMA observations will break new ground in the understanding of dust and molecule production.
Supernova searches and rates
Authors: Cappellaro Enrico 
Published: January 2014

AbstractSupernova statistics, establishing a direct link between stellar populations and explosion scenarios, is a crucial test of stellar evolution theory. Nowadays, a number of SN searches in the local Universe and at high redshifts are allowing observational probes of long standing theoretical scenarios. I will briefly review some of the most interesting results in particular for what concern the evolution with cosmic time of the SN rate, which is one of the topic that in the last few years had a most rapid development.
X-rays from Core-collapse Supernovae
Authors: Pooley David 
Published: January 2014

AbstractCore-collapse supernovae can produce X-rays through a variety of mechanisms, which are briefly reviewed. Through a combination of targeted searches of specific supernovae and archival searches for serendipitous coverage of supernovae, the number of known X-ray supernovae has grown by a factor of five in the past 13 years, when the Chandra X-ray Observatory and XMM-Newton were launched. The Swift satellite has contributed greatly to the discovery of X-ray emitted supernovae, but care must taken with all Swift detections given its spatial resolution and the number of X-ray binaries typically seen in external galaxies. About half of the reported Swift detections of X-ray emission from supernovae are in fact not due to the supernovae but from unrelated nearby sources in the host galaxies.
Radio Observations Of A Nearby Type IIP SN 2012aw
Authors: Yadav Naveen , Ray Alak , Chakraborti Sayan , Stockdale Christopher , Chandra Poonam , Smith Randall , Roy Rupak , Dwarkadas Vikram , Sutaria Firoza , Pooley Dave , Kumar Brijesh , Bose Subhash 
Published: January 2014

AbstractSN 2012AW is a type-IIP supernova which exploded in M95. In this paper we discuss the radio observations of this supernova and model them to determine the important parameters relevant to the explosion and the evolution of blast wave. We also determine the dominant cooling process important to this source.
The optical photometric and spectroscopic investigation of Type IIP supernova 2012A
Authors: Roy Rupak , Sutaria Firoza , Bose Subhash , Johnson Sean , Dwarkadas Vikram , York Brian , Kumar Brijesh , Kumar Brajesh , Bhatt Vijay K. , Chakraborti Sayan , York Don , Ritchey Adam , Saurage Gabrielle , Kaiser Mary Beth 
Published: January 2014

AbstractSupernova 2012A was discovered on 7.39UT, January, 2012 in the nearby galaxy NGC 3239 at an unfiltered magnitude of 14.6 and classified spectroscopically as a Type IIP event. Here, we present the optical photometric and spectroscopic follow-up of the event during 14d to 130d post explosion.
Supernova progenitor mass constraints through spatial correlations with host galaxy star formation
Authors: Anderson Joseph P 
Published: January 2014

AbstractWe present progenitor mass constraints on supernovae (SNe), from correlations with star-forming regions within host galaxies. Through a pixel statistics method used together with H-alpha imaging of host galaxies, we present a progenitor mass sequence running from supernovae type Ia (SNIa) arising from the lowest, through SNII, SNIb, and finally SNIc arising from the highest mass progenitors, implied from an increasing association of their explosion sites with star formation (SF). We also present constraints on the various core-collapse (CC) sub-types, finding the perhaps surprising result that SNIIn show the lowest degree of association with SF of any CC type, implying relatively low-mass progenitors. Finally, we compare the SNIIn environment distribution to that of SNIa, posing the provocative question that additional SNIIn may be linked to the SNIa phenomenon where the latter's spectra are hidden beneath that of circumstellar material (CSM) interaction.
Molecules and dust in the ejecta of Type II-P supernovae
Authors: Cherchneff I. , Sarangi A. 
Published: January 2014

AbstractWe study the formation of molecules and dust clusters in the ejecta of solar metallicity, Type II-P supernovae using a chemical kinetic approach and follow the evolution of molecules and small dust cluster masses from day 100 to day 1500 after explosion. We predict that large masses of molecules including CO, SiO, SiS, O2, and SO form in the ejecta. We show that the non-equilibrium chemistry results in a gradual build up of the dust mass from small (~10−5M⊙) to large values (~5×10−2M⊙) over a five-year period after explosion. This result provides a natural explanation to the discrepancy between the small dust masses detected at infrared wavelengths some 500 days post-explosion and the larger amounts of dust recently detected with the Herschel telescope in supernova remnants.
The Galactic distribution of SNRs
Authors: Green D. A. 
Published: January 2014

AbstractIt is not straightforward to determine the distribution of supernova remnants (SNRs) in the Galaxy. The two main difficulties are that there are observational selection effects that mean that catalogues of SNRs are incomplete, and distances are not available for most remnants. Here I discuss the selection effects that apply to the latest catalogue of Galactic SNRs. I then compare the observed distribution of ‘bright’ SNRs in Galactic longitude with that expected from models in order to constrain the Galactic distribution of SNRs.
Discovery of supernova remnants in the Sino-German λ6 cm polarization survey of the Galactic plane
Authors: Gao X. Y. , Sun X. H. , Han J. L. , Reich W. , Reich P. , Wielebinski R. 
Published: January 2014

AbstractThe Sino-German λ6 cm polarization survey has mapped in total intensity and polarization intensity over an area of approximately 2200 square degrees in the Galactic disk. This survey provides an opportunity to search for Galactic supernova remnants (SNRs) that were previously unknown. We discovered the new SNRs G178.2−4.2 and G25.1−2.3 which have non-thermal spectra, using the λ6 cm data together with the observations with the Effelsberg telescope at λ11 cm and λ21 cm. Both G178.2−4.2 and G25.1−2.3 are faint and have an apparent diameter greater than 1°. G178.2−4.2 shows a polarized shell. HI data suggest that G25.1−2.3 might have a distance of about 3 kpc. The λ6 cm survey data were also very important to identify two other new SNRs, G152.4−2.1 and G190.9−2.2.
The First Systematic Multi-wavelength Survey of Extragalactic Supernova Remnants
Authors: Leonidaki I. , Boumis P. , Zezas A. 
Published: January 2014

AbstractWe present the largest sample of multi-wavelength Supernova Remnants (SNRs) in six nearby galaxies, based on Chandra archival data and deep optical narrow-band Hα and [Sii] images as well as spectroscopic observations. We have identified 37 X-ray selected thermal SNRs, 30 of which are new identifications and ~ 400 optical SNRs, for 67 of which we spectroscopically verified their shock-excited nature. We discuss the properties of the X-ray/optically detected SNRs in different types of galaxies and hence different environments, in order to address their dependence on their Interstellar Medium (ISM). We also discuss the SNR populations in the context of the star formation rate of their host galaxies. We cross-correlate parameters of the optically detected SNRs with parameters of coincident X-ray emitting SNRs in order to understand their evolution and investigate possible selection effects.
X-ray imaging and spectroscopic study of the SNR Kes 73 hosting the magnetar 1E 1841–045
Authors: Kumar H. S. , Safi-Harb S. , Slane P. O. , Gotthelf E. V. 
Published: January 2014

AbstractWe present the first detailed Chandra and XMM-Newton study of the young Galactic supernova remnant (SNR) Kes 73 associated with the anomalous X-ray pulsar (AXP) 1E 1841–045. Images of the remnant in the radio (20 cm), infrared (24 μm), and X-rays (0.5–7 keV) reveal a spherical morphology with a bright western limb. High-resolution Chandra images show bright diffuse emission across the remnant, with several small-scale clumpy and knotty structures filling the SNR interior. The overall Chandra and XMM-Newton spectrum of the SNR is best described by a two-component thermal model with the hard component characterized by a low ionization timescale, suggesting that the hot plasma has not yet reached ionization equilibrium. The soft component is characterized by enhanced metal abundances from Mg, Si, and S, suggesting the presence of metal-rich supernova ejecta. We discuss the explosion properties of the supernova and infer the mass of its progenitor star. Such studies shed light on our understanding of SNRs associated with highly magnetized neutron stars.
Reprise of the Supershells
Authors: Chakraborti Sayan , Ray Alak 
Published: January 2014

AbstractNeutral hydrogen cavities have been detected in the Milky Way for decades and more recently in other nearby star-forming galaxies. It has been suggested that at least a fraction of them may be expanding supershells driven by the combined mechanical feedback from multiple supernovae occurring in an OB association. Yet most extragalactic cavities had neither a demonstrated expansion velocity nor an identified OB association inside them. In this presentation, we will outline how new multiwavelength observations are providing us with systems to test the theory of supershells driven by the mechanical feedback from multiple supernovae. We shall also discuss the consequences of these recent results in the context of supernova feedback, propagating star formation and particle acceleration.
The Supernova – ISM/Star-formation interplay
Authors: Hensler Gerhard 
Published: January 2014

AbstractSupernovae are the most energetic stellar events and influence the interstellar medium by their gasdynamics and energetics. By this, both also affect the star formation positively and negatively. In this paper, we review the complexity of investigations aiming at understanding the interchange between supernova explosions with the star-forming molecular clouds. Commencing from analytical studies the paper advances to numerical models of supernova feedback from superbubble scales to galaxy structure. We also discuss parametrizations of star-formation and supernova-energy transfer efficiencies. Since evolutionary models from the interstellar medium to galaxies are numerous and are applying multiple recipes of these parameters, only a representative selection of studies can be discussed here.
Formation of cold filaments from colliding superbubbles
Authors: Ntormousi Evangelia , Fierlinger Katharina , Burkert Andreas , Heitsch Fabian 
Published: January 2014

AbstractWe present results from numerical simulations of expanding and colliding supershells. These large-scale spherical shocks, created by the combined feedback from several OB stars, are unstable to a number of hydrodynamical instabilities, so they quickly fragment into cold and highly structured clumps. A collision between two large shells can organize these small clumps into very filamentary structures, of tens of parsecs length and less than a parsec thick. In simulations where the flow of stellar material is followed with a tracer quantity, cold structures practically do not contain any enriched material from the OB associations at the time of their creation. In this context then, the clumps are created almost exclusively out of diffuse ISM material, containing almost no wind or supernova matter. Although the mechanism presented here is possibly not the only route for filament creation, this predicted property may help identify regions of sequential star formation.
TeV γ-ray source MGRO J2019+37 : PWN or SNR?
Authors: Saha Lab , Bhattacharjee Pijushpani 
Published: January 2014

AbstractMilagro has recently reported an extended TeV γ-ray source MGRO J2019+37 in the Cygnus region. It is the second brightest TeV source after Crab nebula in their source catalogue. No confirmed counterparts of this source are known although possible associations with several known sources have been suggested. We study leptonic as well as hadronic models of TeV emission within the context of Pulsar Wind Nebulae (PWN) and Supernova Remnant (SNR) type sources, using constraints from multi-wavelength data from observations made on sources around MGRO J2019+37. These include radio upper limit given by GMRT, GeV observations by Fermi-LAT, EGRET and AGILE and very high energy data taken from Milagro. We find that, within the PWN scenario, while both leptonic as well as hadronic models can explain the TeV flux from this source, the GMRT upper limit imposes a stringent upper limit on the size of the emission region in the case of leptonic model. In the SNR scenario, on the other hand, a purely leptonic origin of TeV flux is inconsistent with the GMRT upper limit. At the same time, a dominantly hadronic origin of the TeV flux is consistent with all observations, and the required hadronic energy budget is comparable to that of typical supernovae explosions.
Supernova remnants and the origin of cosmic rays
Authors: Vink Jacco 
Published: January 2014

AbstractSupernova remnants have long been considered to be the dominant sources of Galactic cosmic rays. For a long time the prime evidence consisted of radio synchrotron radiation from supernova remnants, indicating the presence of electrons with energies of several GeV. However, in order to explain the cosmic ray energy density and spectrum in the Galaxy supernova remnant should use 10% of the explosion energy to accelerate particles, and about 99% of the accelerated particles should be protons and other atomic nuclei.Over the last decade a lot of progress has been made in providing evidence that supernova remnant can accelerate protons to very high energies. The evidence consists of, among others, X-ray synchrotron radiation from narrow regions close to supernova remnant shock fronts, indicating the presence of 10-100 TeV electrons, and providing evidence for amplified magnetic fields, gamma-ray emission from both young and mature supernova remnants. The high magnetic fields indicate that the condition for accelerating protons to >1015 eV are there, whereas the gamma-ray emission from some mature remnants indicate that protons have been accelerated.
Simulating the Outer Nebula of SN 1987A
Authors: Fitzpatrick Ben , Morris Thomas , Podsiadlowski Philipp 
Published: January 2014

AbstractAs has been shown previously, the triple-ring nebula around SN 1987A can be understood as a direct consequence of the merger of two stars, some 20,000 yr before the explosion. Here we present new SPH simulations that also include the pre-merger mass loss and show that this may be able to explain other structures observed around SN 1987A, such as Napoleon's hat and various light echoes.
SN 2010as and Transitional Ib/c Supernovae
Authors: Folatelli Gastón 
Published: January 2014

AbstractWe present intensive photometric and spectroscopic observations of SN 2010as carried out by the Millennium Center for Supernova Studies (MCSS) and the Carnegie Supernova Project (CSP). The SN belongs to the transitional type Ibc (SN Ibc) that is characterized by the slow appearance of weak helium lines with low expansion velocities. We find a wide variety of photometric properties among otherwise spectroscopically similar SN Ibc. A hydrodynamical model is used to provide physical properties of SN 2010as in comparison with the bolometric light curve and expansion velocity.
The strange case of SN 2011ja and its host
Authors: Chakraborti Sayan , Ray Alak , Smith Randall , Ryder Stuart , Yadav Naveen , Sutaria Firoza , Dwarkadas Vikram V. , Chandra Poonam , Pooley David , Roy Rupak 
Published: January 2014

AbstractSN 2001ja was observed twice in three months using the Chandra X-Ray Observatory. The X-ray flux could be due to interaction with the circumstellar medium, perhaps dominated by the reverse shock heated thermal plasma, or from inverse Compton scattering at the forward shock. In both cases, for a steady wind-like circumstellar density profile, the X-ray flux is expected to fall off as a power law or faster. But the flux from the position of SN 2011ja, increased by a factor of three between these observations. In this presentation, we investigated possible reasons, including contamination from other astrophysical sources such as a X-Ray Binary, within the Chandra's resolution, in the host galaxy using our observations, modelling and pre-explosion Chandra/XMM data.