bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Stratigraphy of Kirkhead Cave, an Upper Palaeolithic Site in Northern England: Discussion
Authors: Gale S. J. , Hunt C. O. 
Published: February 2014

Volume 52 of the Proceedings of the Prehistoric Society contained two articles (Salisbury 1986; Tipping 1986) critical of our paper ‘The stratigraphy of Kirkhead Cave, an upper palaeolithic site in northern England’ (Gale and Hunt 1985). Here we reply.Before dealing with the criticisms made by Salisbury, we correct the factual errors in his paper.1. Bolton and Morris ‘… excavated through, and ultimately removed some 5 to 7 metres of cave earth…’ (Salisbury 1986, 321). In fact, the reports indicate a maximum depth of excavation of 7 ft (2.1 m) (Bolton 1864, cclii) or 8 ft (2.4 m) (Morris 1865–66, 360, 361; 1866, 169, 170; Bolton 1869, 167–68).2. Bolton and Morris's ‘… publications are of little value today, and both may be considered to have been “bone hunters” and collectors’ (Salisbury 1986, 321). The assertion that Bolton and Morris's excavation reports are of little value suggests that Salisbury is not familiar with the wealth of early literature on this site. The reports provide a picture of a rich and varied assemblage of artefacts and macrofauna in the unit overlying the stalagmite floor in the cave. Information is also provided on the lithology of that unit. Interpretation of these reports allows the reconstruction of the stratigraphic context of the finds: we direct Salisbury's attention to Gale and Hunt (1985, 296–97) for an indication of the stratigraphic reconstruction possible from the information given in these early publications.
From Foraging to Food Production in South-east Ireland: Some Lithic Evidence
Authors: Peterson Jane D. 
Published: February 2014

Current models for the transition from foraging to food production in Ireland describe a range of possibilities concerning the roles played by indigenous populations, the length of overlap between the adaptive systems and the potential influence of one group on the other. For example, Woodman views Mesolithic populations as passive and temporally discrete for the most part (1976; 1978c; 1987). Alternatively, Aalen (1978) sees the potential for Mesolithic groups exerting a significant influence on the Neolithic populations. In Case's model, Neolithic lifeways are introduced fully formed into Ireland, with little or no input from indigenous groups (1969; 1976).All three agree that colonists initiated the transition on the island. Expanding these models and outlining expectations based on them provides the baseline against which the data from Waterford will be measured.
A Vase à Anse from Guernsey in the Channel Islands
Authors: Nilen Helen A. L. 
Published: February 2014

Tomalin (1988) commented on the similarities of vases a anses in Jersey to those in both north Brittany and south Britain. However following earlier writers, including Kendrick (1928, 89) and Hawkes (1938, 112), who also noted these vessels in Jersey, he finds no examples from the rest of the Channel Islands. Interestingly Kendrick illustrates a single-handled vase à anse from the site of La Rocque qui Sonne, Guernsey (1928, pl. XIV, G80); he describes it simply as a ‘small globular cup’ with ribbon handle (1928, 164). Presumably the Guernsey vessel's single handle excluded it from Kendrick's class ‘I’ of ‘Biconical vases with ribbon handles’ from Jersey, which he identified as ‘familiar Bronze Age ware in Brittany’ (1928, 89).The finding of vases à anses in the Channel Islands indicates communication with at least Brittany, though at a period when the islands seem to have had little to offer the visitor, being at a date just prior to an apparent cessation of contact with Armorican ‘exchange partners’ of long standing. Briard (1986) used the vases à anses among other artefacts, to stress such contacts between the islands and Brittany during the Later Neolithic and Early Bronze Age.
The Prehistoric Society: From East Anglia to the
World
Authors: Clark Grahame 
Published: February 2014

It is doubly appropriate that the Prehistoric Society should celebrate its
jubilee in Norwich. The Society was born in the Castle on 23 February 1935
of a parent conceived improbably enough in the Public Library at a meeting
held on 26 October 1908 to inaugurate an East Anglian Society ‘for the study
of all matters appertaining to prehistoric man’. The question I want you to
consider in this address is how the Prehistoric Society of East Anglia
developed so rapidly to the point at which it achieved national status as
The Prehistoric Society. Let me begin by removing one misapprehension. My
hands are not dripping with East Anglian blood nor have I just wiped them
clean. The Prehistoric Society was not the outcome of a revolutionary
putsch. It stemmed from nothing more dramatic than a recognition that the
Prehistoric Society had long ceased to be East Anglian. When we met at
Norwich Castle for our Annual General Meeting in 1935 and passed the
resolution which eliminated the words ‘of East Anglia’ from our title we
were merely recognizing a fact, that we had long ceased to be East Anglian
in anything but name. There were no dissentient votes.The two men who between them set the Prehistoric Society on its feet came
from different but complementary backgrounds. W. G. Clarke was Norfolk born
and bred and earned his living as a working journalist in Norwich, while
cultivating a wide-ranging interest in natural history and prehistoric
archaeology.
A personal view of the scientific career of Wojtek Dziembowski (perceived by an admirer from abroad)
Authors: Gough Douglas 
Published: February 2014

AbstractI present a personal view of Wojtek Dziembowski's scientific career, derived mainly from my direct interactions with Wojtek. Necessarily this presentation is biased towards the earlier days, partly because we interacted more then, and partly because the presentation after mine is by a local admirer who has been much more involved than I with Wojtek's later work.
What can we expect from precision asteroseismology?
Authors: Handler G. 
Published: February 2014

AbstractPrecision asteroseismology is the determination of accurate stellar parameters from oscillation data. At first successful for pulsating white dwarf stars, it is now applied to more and more types of stars. We give a number of selected examples where precision asteroseismology, but also asteroseismology based on few observables may lead to considerable improvement of stellar astrophysics in the near future.
A review of pulsating stars from the ASAS data
Authors: Pigulski Andrzej 
Published: February 2014

AbstractThe All-Sky Automated Survey (ASAS) appeared to be extremely useful in establishing the census of bright variable stars in the sky. A short review of the characteristics of the ASAS data and discoveries based on these data and related to pulsating stars is presented here by an enthusiastic user of the ASAS data.
On the new late B- and early A-type periodic variable stars
Authors: Mowlavi Nami , Saesen Sophie , Barblan Fabio , Eyer Laurent 
Published: February 2014

AbstractWe summarize the properties of the new periodic, small-amplitude, variable stars recently discovered in the open cluster NGC 3766. They are located in the region of the Hertzsprung-Russell diagram between δ Sct and slowly pulsating B stars, a region where no sustained pulsation is predicted by standard models. The origin of their periodic variability is currently unknown. We also discuss how the Gaia mission, launched at the end of 2013, can contribute to our knowledge of those stars.
Some highlights of the latest CoRoT results on stellar physics
Authors: Deheuvels S. ,   the CoRoT team
Published: February 2014

AbstractSince its launch in December 2006, the CoRoT satellite has provided photometric data precise down to the micro-magnitude level for about 150 bright stars and 150 000 fainter ones. These stars have been observed over runs covering up to 160 days with a 90% duty cycle. Seismic data of such precision had been longed for by the scientific community for decades, and expected as a way of making progress in our understanding of stellar structure and evolution. The analysis and interpretation of CoRoT seismic data have indeed made it possible to place observational constraints on several key aspects of stellar structure and evolution, such as the size of mixed convective cores, magnetic activity, mass loss. . . We here present some highlights of the CoRoT results and their implications in terms of internal stellar structure.
Subtle flickering in Cepheids: Kepler and MOST
Authors: Evans Nancy Remage , Szabó Robert , Szabados Laszlo , Derekas Aliz , Matthews Jaymie M. , Cameron Chris ,   the MOST Team
Published: February 2014

AbstractFundamental mode classical Cepheids have light curves which repeat accurately enough that we can watch them evolve (change period). The new level of accuracy and quantity of data with the Kepler and MOST satellites probes this further. An intriguing result was found in the long time-series of Kepler data for V1154 Cyg the one classical Cepheid (fundamental mode, P = 4.9 d) in the field, which has short term changes in period (≃20 minutes), correlated for ≃10 cycles (period jitter). To follow this up, we obtained a month long series of observations of the fundamental mode Cepheid RT Aur and the first overtone pulsator SZ Tau. RT Aur shows the traditional strict repetition of the light curve, with the Fourier amplitude ratio R1/R2 remaining nearly constant. The light curve of SZ Tau, on the other hand, fluctuates in amplitude ratio at the level of approximately 50%. Furthermore prewhitening the RT Aur data with 10 frequencies reduces the Fourier spectrum to noise. For SZ Tau, considerable power is left after this prewhitening in a complicated variety of frequencies.
Stellar Observations Network Group: The prototype is nearly ready
Authors: Grundahl Frank , Christensen-Dalsgaard Jørgen , Pallé Pere L. , Andersen Mads F. , Frandsen Søren , Harpsøe Kennet , Jørgensen Uffe Gråe , Kjeldsen Hans , Rasmussen Per K. , Skottfelt Jesper , Sørensen Anton N. , Hage Andrea Triviño 
Published: February 2014

AbstractThe prototype telescope and instruments for the Stellar Observations Network Group (SONG) are nearing completion at the Observatorio del Teide on Tenerife. In this contribution we describe the current status (autumn 2013) of the telescope and its instrumentation. Preliminary performance characteristics are presented for the high-resolution spectrograph based on daytime observations of the Sun and a 4 hour test series obtained for the sub-giant β Aquilae.
Extracting oscillation frequencies from data: various approaches
Authors: Engelbrecht C. A. 
Published: February 2014

AbstractAsteroseismology depends absolutely on the detection of authentic pulsation signatures in stars. A variety of mathematical and statistical tools have been developed to extract such signatures from photometric and spectroscopic time series. The earliest tools were developed on the platform of Fourier analysis, and Fourier-based methodology still plays a major part in the detection of pulsation signatures in the present day. Alternative approaches have been gaining ground in recent years. This article offers a brief but broad review of the various methodologies for detecting authentic periodic signals that have been developed over the past few decades, including examples of their pitfalls and successes.
Identification of pulsation modes from photometry
Authors: Breger Michel 
Published: February 2014

AbstractThe identification of the detected pulsation modes in terms of the spherical harmonic quantum numbers is crucial for asteroseismology. Light curves obtained in different passbands have become an important tool for mode identifications, which rely on wavelength-dependent amplitudes and phase shifts. We demonstrate this for different types of pulsators and review recent successes from earth-based measurements, especially in determining the important l values. The extensive amount of accurate data needed to determine small phase shifts and accurate amplitude ratios suggests multicolor measurements using space satellites. This motivated the multicolor BRITE satellite project, for which the first two satellites have already been launched successfully. We demonstrate the potential from models computed for the BRITE wavelengths. Most of the excellent presently available satellite photometry is not multicolor, although frequencies with amplitudes as small as a few parts-per-million have been detected and confirmed. We briefly discuss mode identifications from frequency patterns, including the use of correlations between phase and amplitude changes.
Distance determination from the Cepheid and RR Lyrae period-luminosity relations
Authors: Ngeow Chow-Choong , Gieren Wolfgang , Klein Christopher 
Published: February 2014

AbstractCepheids and RR Lyrae stars are important pulsating variable stars in distance scale work because they serve as standard candles. Cepheids follow well-defined period-luminosity (PL) relations defined for bands extending from optical to mid-infrared (MIR). On the other hand, RR Lyrae stars also exhibit PL relations in the near-infrared and MIR wavelengths. In this article, we review some of the recent developments and calibrations of PL relations for Cepheids and RR Lyrae stars. For Cepheids, we discuss the calibration of PL relations via the Galactic and the Large Magellanic Cloud routes. For RR Lyrae stars, we summarize some recent work in developing the MIR PL relations.
Pulsating stars as stellar population tracers
Authors: Clementini Gisella 
Published: February 2014

AbstractPulsating stars of different types are in different evolutionary phases, thus allowing one to trace stellar components of different age in the host systems. The light variation caused by the cyclic expansion/contraction of the surface layers makes a pulsating star much easier to identify than constant stars in the same evolutionary phase. Pulsating stars thus offer a powerful tool to disentangle the various stellar generations in systems where stars of different age and metal abundance populate the same regions of the colour-magnitude diagram. An overview is presented of how pulsating stars can be used as tools to study the stellar populations, and the structure and formation process in Local Group galaxies.
The Araucaria Project: the Baade-Wesselink projection factor of pulsating stars
Authors: Nardetto Nicolas , Storm Jesper , Gieren Wolfgang , Pietrzyński Grzegorz , Poretti Ennio 
Published: February 2014

AbstractThe projection factor used in the Baade-Wesselink method of determining the distance of Cepheids makes the link between stellar physics and the cosmological distance scale. A coherent picture of this physical quantity is now provided based on several approaches. We present the latest news on the expected projection factor for different kinds of pulsating stars in the Hertzsprung-Russell diagram.
The position of confirmed pre-main sequence pulsators in the H-R diagram and an overview of their properties
Authors: Zwintz Konstanze , Casey Mike , Guenther David 
Published: February 2014

AbstractPre-main sequence (PMS) stars can become vibrationally unstable during their evolution to the zero-age main sequence (ZAMS). As they gain their energy from gravitational contraction and have not started nuclear fusion in their cores yet, their inner structures are significantly different to those of (post-) main sequence stars and can be probed by asteroseismology.Using photometric time series from ground and from space (MOST, CoRoT & Spitzer) the number of confirmed pulsating pre-main sequence stars has increased significantly within the last years and allowed to find members of new classes of PMS pulsators. Apart from the well-established group of δ Scuti type PMS stars, members of the groups of PMS γ Doradus, PMS δ Scuti – γ Doradus hybrid and PMS slowly pulsating B (SPB) stars have been discovered. For five PMS δ Scuti candidates, space photometry has revealed that they only show irregular variability, but no pulsations.The unique high-precision space data were combined with dedicated high-resolution spectra to probe the parameter space in the H-R diagram and study the properties of PMS pulsators in comparison to their evolutionary stage.
Atomic diffusion and element mixing in pulsating stars
Authors: Alecian Georges 
Published: February 2014

AbstractStellar plasmas are multicomponent anisotropic gases. Each component (chemical element) of these gases experiences specific forces related to its properties, which leads each element to diffuse with respect to the others. There is no reason why a stellar plasma should remain homogeneous except if mixing motions enforce homogeneity. Because atomic diffusion is a very slow process, the element separation only occurs in places where mixing motions are weak enough not to erase the effect of the ineluctable tendency of chemical elements to migrate. In this talk, I will present how atomic diffusion and mixing processes compete in stars (interiors as well as atmospheres), and I will show various cases where atomic diffusion is believed to have noticeable effects. This concerns several types of stars throughout the H-R diagram, including pulsating ones.
Asteroseismic signatures of magnetic activity variations in solar-type stars
Authors: Metcalfe Travis S. 
Published: February 2014

AbstractObservations of magnetic activity cycles in other stars provide a broader context for our understanding of the 11-year sunspot cycle. The discovery of short activity cycles in a few stars, and the recognition of analogous variability in the Sun, suggest that there may be two distinct dynamos operating in different regions of the interior. Consequently, there is a natural link between studies of magnetic activity and asteroseismology, which can characterize some of the internal properties that are relevant to dynamos. I provide a brief historical overview of the connection between these two fields (including prescient work by Wojtek Dziembowski in 2007), and I highlight some exciting results that are beginning to emerge from the Kepler mission.
RR Lyrae studies with Kepler: showcasing RR Lyr
Authors: Kolenberg Katrien , Kurucz Robert L. , Stellingwerf Robert , Nemec James M. , Moskalik Paweł , Fossati Luca , Barnes Thomas G. 
Published: February 2014

AbstractFour years into the Kepler mission, an updated review on the results for RR Lyrae stars is in order. More than 50 RR Lyrae stars in the Kepler field are observed with Kepler and each one of them can provide us with new insight into this class of pulsating stars. Ground-based spectroscopy of the Kepler targets allows us to narrow down their physical parameters. Previously, we already reported a 50% occurrence rate of modulation in the RRab stars, a large variety of modulation behavior, period doubling in several Blazhko stars, the detection of higher- overtone radial modes, probable non-radial modes and new types of multiple-mode RR Lyrae pulsators, among both the RRab and the RRc stars. In addition, the quasi-continuous photometry obtained over several years with Kepler allows one to observe changes in Blazhko behavior and additional longer cycles. These observations have sparked new theoretical modelling efforts. In this short paper we showcase RR Lyr itself. The star has been observed with Kepler in short cadence, and some remarkable features of its pulsation behavior are unveiled in this long-studied prototype, through the Kepler photometry and additional spectroscopic data.
The most massive pulsating white dwarf stars
Authors: Castanheira Barbara G. , Kepler S. O. 
Published: February 2014

AbstractMassive pulsating white dwarf stars are extremely rare, because of their small size and because they are the final product of high-mass stars, which are less common. Because of their intrinsic smaller size, they are fainter than the normal size white dwarf stars. The motivation to look for this type of stars is to be able to study in detail their internal structure and also derive generic properties for the sub-class of variables, the massive ZZ Ceti stars. Our goal is to investigate whether the internal structures of these stars differ from the lower-mass ones, which in turn could have been resultant from the previous evolutionary stages.In this paper, we present the ensemble seismological analysis of the known massive pulsating white dwarf stars. Some of these pulsating stars might have substantial crystallized cores, which would allow us to probe solid physics in extreme conditions.
Origin and pulsation of hot subdwarfs
Authors: Randall S. K. , Fontaine G. , Charpinet S. , Van Grootel V. , Brassard P. 
Published: February 2014

AbstractWe briefly introduce hot subdwarfs and their evolutionary status before discussing the different types of known pulsators in more detail. Currently, at least six apparently distinct types of variable are known among hot subdwarfs, encompassing p- as well as g-mode pulsators and objects in the Galactic field as well as in globular clusters. Most of the oscillations detected can be explained in terms of an iron opacity mechanism, and quantitative asteroseismology has been very successful for some of the pulsators. In addition to helping constrain possible evolutionary scenarios, studies focussing on stellar pulsations have also been used to infer planets and characterize the rotation of the host star.
Reaching the 1% accuracy level on stellar mass and radius determinations from asteroseismology
Authors: Van Grootel V. , Charpinet S. , Fontaine G. , Brassard P. , Green E. M. 
Published: February 2014

AbstractAsteroseismic modeling of subdwarf B (sdB) stars provides measurements of their fundamental parameters with a very good precision; in particular, the masses and radii determined from asteroseismology are found to typically reach a precision of 1% containing various uncertainties associated with their inner structure and the underlying microphysics (composition and transition zones profiles, nuclear reaction rates, etc.). Therefore, the question of the accuracy of the stellar parameters derived by asteroseismology is legitimate. We present here the seismic modeling of the pulsating sdB star in the eclipsing binary PG 1336–018, for which the mass and the radius are independently and precisely known from the modeling of the reflection/irradiation effect and the eclipses observed in the light curve. This allows us to quantitatively evaluate the reliability of the seismic method and test the impact of uncertainties in our stellar models on the derived parameters. We conclude that the sdB star parameters inferred from asteroseismology are precise, accurate, and robust against model uncertainties.
Being rich helps – the case of the sdBV KIC 10670103
Authors: Krzesinski Jurek , Bachulski Szymon 
Published: February 2014

AbstractWe present a study of KIC 10670103, a pulsating hot subdwarf in the Kepler field. By means of Fourier analysis, we investigate periodic signals associated with pulsations. Using asymptotic relationships and rotational multiplets we identify degrees of modes. The Fourier spectrum appears to be rich in l=1 and l=2 multiplets allowing derivation of a ~90-day rotation period of the star from rotational splittings. Comparing the identified gravity-mode period spacing pattern with theoretical models we show that KIC 10670103 has to be a thick-envelope sdBV.