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Conventional wisdom since the earliest studies of Irish English has attributed much of what is distinctive about this variety to the influence of the Irish language. From the early philologists (Joyce 1910, van Hamel 1912) through the classic works of Henry (1957, 1958) and Bliss (1979) down to present-day linguistic orientations (e.g. Corrigan 2000 a, Filppula 1999, Fiess 2000, Hickey 2000, Todd 1999, and others), the question of Irish-language influence may be disputed on points of detail, but remains a central focus for most studies in the field. It is not our intention to argue with this consensus, nor to examine specific points of grammar in detail, but, rather, to suggest an approach to this question which (a) takes for its empirical base a sample of the standard language, rather than dialectal material or the sample sentences so beloved of many papers on the subject, and (b) understands Celticity not just in terms of the formal transfer of grammatical features, but as an indexical feature of language use, i.e. one in which English in Ireland is used in such a way as to point to the Irish language as a linguistic and cultural reference point. In this sense, our understanding of Celticity is not entirely grammatical, but relies as well on Pierce’s notion of indexicality (see Greenlee 1973), by which semiotic signs ‘point to’ other signs. Our focus in assessing Celticity, then, derives in the first instance from an examination of the International Corpus of English (ICE). We have recently completed the publication of the Irish component of ICE (ICE-Ireland), a machinereadable corpus of over 1 million words of speech and writing gathered from a range of contexts determined by the protocols of the global International Corpus of English project. The international nature of this corpus project makes for ready comparisons with other varieties of English, and in this paper we will focus on comparisons with the British corpus, ICE-GB. For references on ICE generally, see Greenbaum 1996; for ICE-GB, see especially Nelson, Wallis and Aarts 2002; and for ICE-Ireland, see papers such as Kirk, Kallen, Lowry & Rooney (2003), Kirk & Kallen (2005), and Kallen & Kirk (2007). Our first approach will be to look for signs of overt Celticity in those grammatical features of Irish English which have been put forward as evidence of Celtic transfer (or of the reinforcement between Celtic and non-Celtic historical sources); our second approach will be to look at non-grammatical ways in which texts in ICEIreland become indexical of Celticity by less structural means such as loanwords, code-switching, and covert reference using ‘standard’ English in ways that are specific to Irish usage. We argue that, at least within the standard language as we have observed it, Celticity is at once less obvious than a reading of the dialectal literature might suggest and, at the same time, more pervasive than a purely grammatical approach would imply.
Extract: [...]The New English Dictionary, later to become the Oxford English Dictionary, was first published between 1884 and 1928. To add new material, two supplements were issued after this, the first in 1933, and another, more extensive one between 1972 and 1986. In 1989, the Oxford English Dictionary, second edition (OED2) was published, which integrated the material from the original dictionary and the supplements into a single alphabetical sequence. However, virtually all material contained in this edition still remained in the form in which it was originally published. This is the edition most commonly used today, as it forms the basis of the Oxford English Dictionary Online and is also still being sold in print and on CD-ROM. In 1991, a new project started to revise the entire dictionary and bring its entries up to date, both in terms of English usage and in terms of associated scholarship, such as encyclopaedic information and etymologies. The scope was also widened, placing a greater emphasis on English spoken outside Britain. The revision of the dictionary began with the letter M, and the first updated entries were published online in March 2000 (OED3). Quarterly publication of further material has extended the range of revised entries as far as PROTEOSE n. (June 2007). New words from all parts of the alphabet have been published alongside the regular revision.[...]
Extract: [...]Intriguing as they undoubtedly are, the early sixteenth-century lists of books in the Earl of Kildare’s library may well have inadvertently helped to lull scholars into visualising a rather idealised picture of language balance in multilingual late medieval Ireland. The lists reflect a society in which the four languages, Irish, English, Latin and French, vied as scholarly media and where the outcome in the Earl’s library was a four-way photo-finish. The number of volumes in each of the languages was recorded as follows: Latin, 34; French, 35; English, 22; Irish, 20 (Mac Niocaill 1992: 312-314). But of course the multilingual contact situation in Ireland had always been quite dynamic, both at vernacular and at scholarly levels, following the Anglo-Norman invasion of 1169. Although French continued to be employed in official documents into the second half of the 15th century, it had already ceded its vernacular role to English in the towns of the colonists prior to the drawing up of the Statutes of Kilkenny in 1366. These Statutes, composed in Norman-French, the primary language of English law at the time, provide an earlier snapshot of the language situation within the areas under English jurisdiction, as they sought to compel the colonists to desist from adopting Irish as a community vernacular. Ironically, no mention is made of Norman-French in the Statutes themselves. It is clear that what was at issue was a contest for supremacy between Irish and English as the principal vernacular among the colonists.[...]
Extract: [...]In the first part of this paper I trace the language shift from Breton to French within the historical, social and ideological framework in which it occurred. I then argue that 19th and 20th-century attempts by scholars and militants to rehabilitate the Breton language led to the creation of a unified standard (peurunvan).2 The consequence has been the rise of a three-way diglossic rapport between the speakers of French, the new Breton standard3 and those of the traditional Breton vernaculars. Taking the varieties of southern Cornouaille (Finistère) between Quimper and Quimperlé as a point of comparison,4 I focus on a number of phonological, morphological, syntactical and lexical features which, though far from exhausttive, are not generally taken into account in the new standard language. These details provide a general idea of how varieties of Breton function at the micro-dialectological level, as well as ways in which they can differ from the standard and other spoken varieties. The paper concludes with observations regarding the necessity to consider languages, language varieties and their speakers within relevant social contexts.[...]
Extract: [...] One of the often noted characteristic features of the Celtic languages is the absence of a singular verbal form with the meaning ‘to have’.1 The principal way of expressing possession is through periphrastic constructions with prepositions (such as Irish ag, Scottish Gaelic aig ‘at’; Welsh gan, Breton gant ‘at, with’) and appropriate forms of the substantive verb. Pronominal prepositions, another distinctive feature of the Celtic languages, consist of a preposition and a suffixed pronoun, or rather a pronominal personal ending. This construction may be analyzed as an instance of category fusion. Thus, the Irish and Welsh equivalents of English ‘I have money’ are Tá airgead agam or Mae arian gen i, respectively, both literally meaning ‘is money at-me/with-me’. This note discusses pronominal possessive constructions in Celtic languages (and some comparable examples from Celtic Englishes) and provides some background information on pronominal prepositions and comments on historical developments of these forms. It also discusses some terminological issues involved in labelling the construction in question. [...]
Extract: That the Celtic languages were of the Indo-European family was first recognised by Rasmus Christian Rask (*1787), a young Danish linguist, in 1818. However, the fact that he wrote in Danish meant that his discovery was not noted by the linguistic establishment until long after his untimely death in 1832. The same conclusion was arrived at independently of Rask and, apparently, of each other, by Adolphe Pictet (1836) and Franz Bopp (1837). This agreement between the foremost scholars made possible the completion of the picture of the spread of the Indo-European languages in the extreme west of the European continent. However, in the Middle Ages the speakers of Irish had no awareness of any special relationship between Irish and the other Celtic languages, and a scholar as linguistically competent as Cormac mac Cuillennáin (†908), or whoever compiled Sanas Chormaic, treated Welsh on the same basis as Greek, Latin, and the lingua northmannorum in the elucidation of the meaning and history of Irish words. [...]
Contents: The Sociolinguistic Conditions favourable to spread of Structural Features Contact-induced Changes in Insular Celtic Phonological Changes The Lenition of Voiceless Stops Raising / i-Affection Lowering / a-Affection Apocope Syncope Morphological The Loss of Case Inflection of Personal Pronouns The Creation of the Equative Degree The Creation of the Imperfect Tense The Creation of the Conditional Mood Morphosyntactic and Syntactic The Creation of Preposed Definite Articles
Extract: [...]The Roman conquest of what was to become the province of Gallia Narbonensis in the second and then of the whole of Transalpine Gaul in the first century B.C. led to the incorporation into the Roman empire of a large part of the territory in which Gaulish was then spoken.1 In consequence, the vernacular rapidly lost its footing at least in public life and was soon replaced by Latin, the language of the new masters, which enjoyed higher prestige (cf. e.g. Meid 1980: 7-8). On the other hand, Gaulish continued to be written for some three centuries and was probably used in speech even longer, especially in rural areas. We must therefore posit a prolonged period of bilingualism. The effects of this situation on the Latin spoken in the provinces of Gaul seem to have been rather limited. A number of lexical items, mostly from the field of everyday life, and some phonetic characteristics are the sole testimonies of a Gaulish substratum in the variety of Latin that was later to develop into the Romance dialects of France (cf. Meid 1980: 38, fn. 77). [...]
Celtic and Afro-Asiatic
(2007)
Extract: [...]It is not remarkable that structural similarities between the Insular Celtic and some Afro-Asiatic1 languages continue to exert a fascination on many people. Research into any language may be enlightening with regard to the understanding of all languages, and languages that show similar features are particularly likely to provide useful information. It is remarkable that the structural similarities between Insular Celtic and Afro-Asiatic languages continue to be interpreted as diagnostic of some sort of special relationship between them; some sort of affinity or mutual affiliation that goes beyond the fact that they are two groups of human languages. This paper investigates again the fallacious nature of the arguments for the Afro-Asiatic/Insular Celtic contact theory (henceforth AA/IC contact theory). It takes its point of departure from Gensler (1993). That work is as yet unpublished, but has had considerable resonance. Such statements as the following indicate the importance that has been attached to the work: “After the studies of Morris-Jones, Pokorny, Wagner2 and Gensler it seems impossible to deny the special links between Insular Celtic and Afro-Asiatic” (Jongeling 2000:64). And the ideas in question have been propagated in the popular scientific press,3 with the usual corollary that it is these ideas that are perceived by the interested but non-specialist public as being at the cutting edge of sound new research, when in fact they may simply be recycled ideas of a discredited theory. For these reasons it is appropriate to subject Gensler’s unpublished work to detailed critique.4 In particular, with regard to the twenty features of affinity between Insular Celtic and Afro-Asiatic which Gensler investigated, it will be shown (yet again, in some cases): [...]
Extract: [...]In Celtic languages (both Continental and Insular) we can find words with uncertain etymology which presumably represent loanwords from other language-families. One can see the traces of the pre-Indo-European substratum of Central and Western Europe, “an original non-Celtic/non-Germanic North West block” according to Kuhn (1961). But we may suppose that this conclusion is not sufficiently justified. This problem can have many different solutions, and we may never be in a position to resolve it definitively.[...]
Small livestock is an important resource for rural human populations in dry climates. How strongly will climate change affect the capacity of the rangeland? We used hierarchical modelling to scale quantitatively the growth of shrubs and annual plants, the main food of sheep and goats, to the landscape extent in the eastern Mediterranean region. Without grazing, productivity increased in a sigmoid way with mean annual precipitation. Grazing reduced productivity more strongly the drier the landscape. At a point just under the stocking capacity of the vegetation, productivity declined precipitously with more intense grazing due to a lack of seed production of annuals. We repeated simulations with precipitation patterns projected by two contrasting IPCC scenarios. Compared to results based on historic patterns, productivity and stocking capacity did not differ in most cases. Thus, grazing intensity remains the stronger impact on landscape productivity in this dry region even in the future.
Excerpt: The shrill sounds of the now seemingly outdated controversy between Gershom Scholem and Martin Buber at the beginning of the sixties are still in the minds of every student of Hasidic literature and thought. - The "Scholem-community" feels content and the "Buber-community" upset. We can summarize the case in a few words. Martin Buber, the pioneer of Hasidism in the Western World, held the position that whoever would want to understand Hasidism had to turn to Hasidic tale as here, in the tales of the Hasidim, real Hasidic life was to be found. Whereas in the Hasidic homilies we meet mere non-creative tradition especially in the form of Kabbalah. Buber did not totally deny the importance of the Hasidic Midrash but he regarded it just as a commentary, i.e. as secondhand material, whereas, in his view, the tale was a true mirror of real Hasidic life [...]
A multitype Dawson-Watanabe process is conditioned, in subcritical and critical cases, on non-extinction in the remote future. On every finite time interval, its distribution is absolutely continuous with respect to the law of the unconditioned process. A martingale problem characterization is also given. Several results on the long time behavior of the conditioned mass process - the conditioned multitype Feller branching diffusion - are then proved. The general case is first considered, where the mutation matrix which models the interaction between the types, is irreducible. Several two-type models with decomposable mutation matrices are analyzed too .
Excerpt: Hasidic Ashkenazi literature is known to scholars of Jewish religion as one of the most prolific sources of medieval Jewish magic or magical beliefs. This is all the more astonishing as the non esoteric writings of the Hasidey Ashkenaz represent a rather traditional Jewish piety as known to us from talmudic sources. Considering this duality of an almost traditional Jewish piety on the one hand and very distinct magic tenets on the other, we may ask whether the Hasidey Ashkenaz themselves perceived any difference between magic and religion. There are indeed a number of modern historians of religion who completely deny the validity of such a distinction, for in most historical religions magic and religion are in fact intertwined to a certain degree, thus permitting almost no differentiation between the two.
Excerpt: The writings from the thirteenth century called by Gershom Scholem the "Writings of the 'lyyun circle" are one of the most intriguing chapters of early kabbalah - this I need not to elaborate on as it is a well known fact to anyone whoever had read these texts or the literature about them. When reading these texts, one gets the impression as if the authors had at hand a box full of terms and phrases into which everybody could just stick his hand and take terms and phrases out of it in order to arrange them according to his own taste, disregarding the meaning they have in the writings of his fellow kabbalists. The result was, that we now have before us a large number of varying mosaic pictures in which we detect again and again the same mosaic pebbles, however composed differently.
Rapid and robust characterization of large earthquakes in terms of their spatial extent and temporal duration is of high importance for disaster mitigation and early warning applications. Backtracking of seismic P-waves was successfully used by several authors to image the rupture process of the great Sumatra earthquake (26.12.2004) using short period and broadband arrays. We follow here an approach of Walker et al. to backtrack and stack broadband waveforms from global network stations using traveltimes for a global Earth model to obtain the overall spatio-temporal development of the energy radiation of large earthquakes in a quick and robust way. We present results for selected events with well studied source processes (Kokoxili 14.11.2001, Tokachi-Oki 25.09.2003, Nias 28.03.2005). Further, we apply the technique in a semi-real time fashion to broadband data of earthquakes with a broadband magnitude >= 7 (roughly corresponding to Mw 6.5). Processing is based on first automatic detection messages from the GEOFON extended virtual network (GEVN).
We use seismic array methods (semblance analysis) to image areas of seismic energy release in the Sunda Arc region and world-wide. Broadband seismograms at teleseismic distances (30° ≤ Δ ≤ 100°) are compared at several subarrays. Semblance maps of different subarrays are multiplied. High semblance tracked over long time (10s of second to minutes) and long distances indicate locations of earthquakes. The method allows resolution of rupture characteristics important for tsunami early warning: start and duration, velocity and direction, length and area. The method has been successfully applied to recent and historic events (M>6.5) and is now operational in real time. Results are obtained shortly after source time, see http://www.geo.uni-potsdam.de/Forschung/Geophysik/GITEWS/tsunami.htm). Comparison of manual and automatic processing are in good agreement. Computational effort is small. Automatic results may be obtained within 15 - 20 minutes after event occurrence.
Team diversity
(2007)
Team diversity refers to the differences between team members on any attribute that may lead each single member of the group to perceive any other member of the group as being different from the self of this particular member. These attributes and perceptions refer to all dimensions people can differ on, such as age, gender, ethnicity, religious and functional background, personality, skills, abilities, beliefs, and attitudes.
Receiver functions are a good tool to investigate the seismotectonic structure beneath the a seismic station. In this study we apply the method to stations situated on or near Sumatra to find constraints on a more detailed velocity model which should improve earthquake localisation. We estimate shallow Moho-depths (~ 21 km) close to the trench and depths of ~30 km at greater distances. First evidences for the dip direction of the slab of ~60° are provided. Receiver functions were calculated for 20 stations for altogether 110 earthquakes in the distance range between 30° and 95° from the receiver. However the number of receiver functions per station is strongly variable as it depends on the installation date, the signal-to-noise-ratio of the station and the reliability of the acquisition.
The authors used the frameworks of reciprocal determinism and occupational socialization to study the effects of work characteristics (consisting of control and complexity of work) on personal initiative (PI)--mediated by control orientation (a 2nd-order factor consisting of control aspiration, perceived opportunity for control, and self-efficacy) and the reciprocal effects of PI on changes in work characteristics. They applied structural equation modeling to a longitudinal study with 4 measurement waves (N = 268) in a transitional economy: East Germany. Results confirm the model plus 1 additional, nonhypothesized effect. Work characteristics had a synchronous effect on PI via control orientation (full mediation). There were also effects of control orientation and of PI on later changes in work characteristics: As predicted, PI functioned as partial mediator, changing work characteristics in the long term (reciprocal effect); unexpectedly, there was a 2nd reciprocal effect of an additional lagged partial mediation of control orientation on later work characteristics.
Observational evidence exists that winds of massive stars are clumped. Many massive star systems are known as non-thermal particle production sites, as indicated by their synchrotron emission in the radio band. As a consequence they are also considered as candidate sites for non-thermal high-energy photon production up to gamma-ray energies. The present work considers the effects of wind clumpiness expected on the emitting relativistic particle spectrum in colliding wind systems, built up from the pool of thermal wind particles through diffusive particle acceleration, and taking into account inverse Compton and synchrotron losses. In comparison to a homogeneous wind, a clumpy wind causes flux variations of the emitting particle spectrum when the clump enters the wind collision region. It is found that the spectral features associated with this variability moves temporally from low to high energy bands with the time shift between any two spectral bands being dependent on clump size, filling factor, and the energy-dependence of particle energy gains and losses.
The most massive stars are those with the shortest but most active life. One group of massive stars, the Luminous Blue Variables (LBVs), of which only a few objects are known, are in particular of interest concerning the stability of stars. They have a high mass loss rate and are close to being instable. This is even more likely as rotation becomes an important factor in stellar evolution of these stars. Through massive stellar winds and sometimes giant eruptions, LBV nebulae are formed. Various aspects in the evolution in the LBV phase lead, beside the large scale morphological and kinematical differences, to a diversity of small structures like clumps, rims, and outflows in these nebulae.
Gamma-rays can be produced by the interaction of a relativistic jet and the matter of the stellar wind in the subclass of massive X-ray binaries known as “microquasars”. The relativistic jet is ejected from the surroundings of the compact object and interacts with cold protons from the stellar wind, producing pions that then quickly decay into gamma-rays. Since the resulting gamma-ray emissivity depends on the target density, the detection of rapid variability in microquasars with GLAST and the new generation of Cherenkov imaging arrays could be used to probe the clumped structure of the stellar wind. In particular, we show here that the relative fluctuation in gamma rays may scale with the square root of the ratio of porosity length to binary separation, $\sqrt{h/a}$, implying for example a ca. 10% variation in gamma ray emission for a quite moderate porosity, h/a ∼ 0.01.
The optical spectrum of Eta Carinae (η Car) is prominent in H I, He i and Fe ii wind lines, all of which vary both in absorption and emission with phase. The phase dependance is a consequence of the interaction between the two objects in the η Car binary (η Car A & B). The binary system is enshrouded by ejecta from previous mass ejection events and consequently, η Car B is not directly observable. We have traced the He i lines over η Car’s spectroscopic period, using HST/STIS data obtained with medium spectral, but high angular, resolving power, and created a radial velocity curve for the system. The He I lines are formed in the core of the system, and appear to be a composite of multiple features formed in spatially separated regions. The sources of their irregular line profiles are still not fully understood, but can be attributed to emission/absorption near the wind-wind interface and/or a direct consequence of the η Car A’s, massive, clumpy wind. This paper will discuss the spectral variability, the narrow emission structure of the He i lines and how clumpiness of the winds may impede the construction of the reliable radial velocity curve, necessary for characterizations of especially η Car B.
The spatially-resolved winds of the massive binary, Eta Carinae, extend an arcsecond on the sky, well beyond the 10 to 20 milliarcsecond binary orbital dimension. Stellar wind line profiles, observed at very different angular resolutions of VLTI/AMBER, HST/STIS and VLT/UVES, provide spatial information on the extended wind interaction structure as it changes with orbital phase. These same wind lines, observable in the starlight scattered off the foreground lobe of the dusty Homunculus, provide time-variant line profiles viewed from significantly different angles. Comparisons of direct and scattered wind profiles observed in the same epoch and at different orbital phases provide insight on the extended wind structure and promise the potential for three-dimensional imaging of the outer wind structures. Massive, long-lasting clumps, including the nebularWeigelt blobs, originated during the two historical ejection events. Wind interactions with these clumps are quite noticeable in spatially-resolved spectroscopy. As the 2009.0 minimum approaches, analysis of existing spectra and 3-D modeling are providing bases for key observations to gain further understanding of this complex massive binary.
The H.E.S.S. collaboration recently reported the discovery of VHE γ-ray emission coincident with the young stellar cluster Westerlund 2. This system is known to host a population of hot, massive stars, and, most particularly, the WR binary WR 20a. Particle acceleration to TeV energies in Westerlund 2 can be accomplished in several alternative scenarios, therefore we only discuss energetic constraints based on the total available kinetic energy in the system, the actual mass loss rates of respective cluster members, and implied gamma-ray production from processes such as inverse Compton scattering or neutral pion decay. From the inferred gammaray luminosity of the order of 1035erg/s, implications for the efficiency of converting available kinetic energy into non-thermal radiation associated with stellar winds in the Westerlund 2 cluster are discussed under consideration of either the presence or absence of wind clumping.
We model the line profile variability (lpv) in spectra of clumped stellar atmospheres using the Stochastic Clump Model (SCM) of the winds of early-type stars. In this model the formation of dense inhomogeneities (clumps) in the line driven winds is considered as being a stochastic process. It is supposed that the emission due to clumps mainly contributes to the intensities of emission lines in the stellar spectra. It is shown that in the framework of the SCM it is possible to reproduce both the mean line profiles and a common pattern of the lpv.
We study the time variability of emission lines in three WNE stars : WR 2 (WN2), WR 3 (WN3ha) and WR152 (WN3). While WR 2 shows no variability above the noise level, the other stars do show variation, which are like other WR stars in WR 152 but very fast in WR 3. From these motions, we deduce a value of β ∼1 for WR 3 that is like that seen in O stars and β ∼2–3 for WR 152, that is intermediate between other WR stars and WR 3.
Luminous Blue Variables show strong changes in their stellar wind on time scales of typically years to decades when they expand and contract radially at approximately constant luminosity. Micro-variability on shorter time scales and amplitudes can be observed superimposed to the larger scale radial changes. I will show long-term time series of high resolution spectra which we have collected in the past 20 years for many of the well known LBVs together with a few time series of weekly sampling (HR Car, R40, R71, R110, R127, S Dor) covering a time windows of up to a few months. Wind variability is seen on short and intermediate time scales with the line profiles changing from P Cygni to inverse P Cygni and double peeked profiles sometimes for the same star and spectral line. On longer time scales the ionisation levels for all chemical elements change drastically due to the strong change of the temperature on the stellar surface. While on the long term the characteristic radial changes may have impact on the over all mass loss rates, the variabilities and asymmetries on short and intermediate time scales may cause false estimates of the mass loss rates when confronting models with the observed line profiles
Hα observations of Rigel obtained on 184 nights during the past ten years with the 1-m telescope and ´echelle spectrograph of Ritter Observatory are surveyed. The line profiles were classified in terms of morphology. About 1/4 of them are of P Cygni type, about 15% inverse P Cygni, about 25% double-peaked, about 1/3 pure absorption, and a few are single emission lines. Transformation of the profile from one type to another typically takes a few days. Although the line stays in absorption for extended intervals, only one high-velocity absorption event of the intensity reported by Kaufer et al. (1996a) was observed, in late 2006. Late in this event, Hα absorption occurred farther to the red than the red wing of a plausible photospheric absorption component, an indication of infalling material. In general, as the absorption events come to an end, the emission typically returns with an inverse P Cygni profile. The Hα profile class shows no obvious correlation with the radial velocity of C II λ6578, a photospheric absorption line.
X-ray spectroscopy is a sensitive probe of stellar winds. X-rays originate from optically thin shock-heated plasma deep inside the wind and propagate outwards throughout absorbing cool material. Recent analyses of the line ratios from He-like ions in the X-ray spectra of O-stars highlighted problems with this general paradigm: the measured line ratios of highest ions are consistent with the location of the hottest X-ray emitting plasma very close to the base of the wind, perhaps indicating the presence of a corona, while measurements from lower ions conform with the wind-embedded shock model. Generally, to correctly model the emerging Xray spectra, a detailed knowledge of the cool wind opacities based on stellar atmosphere models is prerequisite. A nearly grey stellar wind opacity for the X-rays is deduced from the analyses of high-resolution X-ray spectra. This indicates that the stellar winds are strongly clumped. Furthermore, the nearly symmetric shape of X-ray emission line profiles can be explained if the wind clumps are radially compressed. In massive binaries the orbital variations of X-ray emission allow to probe the opacity of the stellar wind; results support the picture of strong wind clumping. In high-mass X-ray binaries, the stochastic X-ray variability and the extend of the stellar-wind part photoionized by X-rays provide further strong evidence that stellar winds consist of dense clumps.
By quantitatively fitting simple emission line profile models that include both atomic opacity and porosity to the Chandra X-ray spectrum of ζ Pup, we are able to explore the trade-offs between reduced mass-loss rates and wind porosity. We find that reducing the mass-loss rate of ζ Pup by roughly a factor of four, to 1.5 × 10−6 M⊙ yr−1, enables simple non-porous wind models to provide good fits to the data. If, on the other hand, we take the literature mass-loss rate of 6×10−6 M⊙ yr−1, then to produce X-ray line profiles that fit the data, extreme porosity lengths – of h∞ ≈ 3 R∗ – are required. Moreover, these porous models do not provide better fits to the data than the non-porous, low optical depth models. Additionally, such huge porosity lengths do not seem realistic in light of 2-D numerical simulations of the wind instability.
We review the effects of clumping on the profiles of resonance doublets. By allowing the ratio of the doublet oscillator strenghts to be a free parameter, we demonstrate that doublet profiles contain more information than is normally utilized. In clumped (or porous) winds, this ratio can lies between unity and the ratio of the f-values, and can change as a function of velocity and time, depending on the fraction of the stellar disk that is covered by material moving at a particular velocity at a given moment. Using these insights, we present the results of SEI modeling of a sample of B supergiants, ζ Pup and a time series for a star whose terminal velocity is low enough to make the components of its Si VIλλ1400 independent. These results are interpreted within the framewrok of the Oskinova et al. (2007) model, and demonstrate how the doublet profiles can be used to extract infromation about wind structure.
We present XMM-Newton Reflection Grating Spectrometer observations of pairs of X-ray emission line profiles from the O star ζ Pup that originate from the same He-like ion. The two profiles in each pair have different shapes and cannot both be consistently fit by models assuming the same wind parameters. We show that the differences in profile shape can be accounted for in a model including the effects of resonance scattering, which affects the resonance line in the pair but not the intercombination line. This implies that resonance scattering is also important in single resonance lines, where its effect is difficult to distinguish from a low effective continuum optical depth in the wind. Thus, resonance scattering may help reconcile X-ray line profile shapes with literature mass-loss rates.
We summarize Chandra observations of the emission line profiles from 17 OB stars. The lines tend to be broad and unshifted. The forbidden/intercombination line ratios arising from Helium-like ions provide radial distance information for the X-ray emission sources, while the H-like to He-like line ratios provide X-ray temperatures, and thus also source temperature versus radius distributions. OB stars usually show power law differential emission measure distributions versus temperature. In models of bow shocks, we find a power law differential emission measure, a wide range of ion stages, and the bow shock flow around the clumps provides transverse velocities comparable to HWHM values. We find that the bow shock results for the line profile properties, consistent with the observations of X-ray line emission for a broad range of OB star properties.
We present one-dimensional, time-dependent models of the clumps generated by the linedeshadowing instability. In order to follow the clumps out to distances of more than 1000 R∗, we use an efficient moving-box technique. We show that, within the approximations, the wind can remain clumped well into the formation region of the radio continuum.
INTEGRAL tripled the number of super-giant high-mass X-ray binaries (sgHMXB) known in the Galaxy by revealing absorbed and fast transient (SFXT) systems. Quantitative constraints on the wind clumping of massive stars can be obtained from the study of the hard X-ray variability of SFXT. A large fraction of the hard X-ray emission is emitted in the form of flares with a typical duration of 3 ksec, frequency of 7 days and luminosity of $10^{36}$ erg/s. Such flares are most probably emitted by the interaction of a compact object orbiting at $\sim10~R_*$ with wind clumps ($10^{22 ... 23}$ g) representing a large fraction of the stellar mass-loss rate. The density ratio between the clumps and the inter-clump medium is $10^{2 ... 4}$. The parameters of the clumps and of the inter-clump medium, derived from the SFXT flaring behavior, are in good agreement with macro-clumping scenario and line-driven instability simulations. SFXT are likely to have larger orbital radius than classical sgHMXB.
Magnetic fields influence the dynamics of hot-star winds and create large scale structure. Based on numerical magnetohydrodynamic (MHD) simulations, we model the wind of θ¹ Ori C, and then use the SEI method to compute synthetic line profiles for a range of viewing angles as function of rotational phase. The resulting dynamic spectrum for a moderately strong line shows a distinct modulation, but with a phase that seems at odds with available observations.
Discussion : X-rays
(2007)
Dynamical simulation of the “velocity-porosity” reduction in observed strength of stellar wind lines
(2007)
I use dynamical simulations of the line-driven instability to examine the potential role of the resulting flow structure in reducing the observed strength of wind absorption lines. Instead of the porosity length formalism used to model effects on continuum absorption, I suggest reductions in line strength can be better characterized in terms of a velocity clumping factor that is insensitive to spatial scales. Examples of dynamic spectra computed directly from instability simulations do exhibit a net reduction in absorption, but only at a modest 10-20% level that is well short of the ca. factor 10 required by recent analyses of PV lines.
The James Webb Space Telescope (JWST) is a large, infrared-optimized space telescope scheduled for launch in 2013. JWST will find the first stars and galaxies that formed in the early universe, connecting the Big Bang to our own Milky Way galaxy. JWST will peer through dusty clouds to see stars forming planetary systems, connecting the MilkyWay to our own Solar System. JWST’s instruments are designed to work primarily in the infrared range of 1 - 28 μm, with some capability in the visible range. JWST will have a large mirror, 6.5 m in diameter, and will be diffraction-limited at 2 μm (0.1 arcsec resolution). JWST will be placed in an L2 orbit about 1.5 million km from the Earth. The instruments will provide imaging, coronography, and multi-object and integral-field spectroscopy across the 1 - 28 μm wavelength range. The breakthrough capabilities of JWST will enable new studies of massive star winds from the Milky Way to the early universe.
Clumps in hot star winds can originate from shock compression due to the line driven instability. One-dimensional hydrodynamic simulations reveal a radial wind structure consisting of highly compressed shells separated by voids, and colliding with fast clouds. Two-dimensional simulations are still largely missing, despite first attempts. Clumpiness dramatically affects the radiative transfer and thus all wind diagnostics in the UV, optical, and in X-rays. The microturbulence approximation applied hitherto is currently superseded by a more sophisticated radiative transfer in stochastic media. Besides clumps, i.e. jumps in the density stratification, so-called kinks in the velocity law, i.e. jumps in dv/dr, play an eminent role in hot star winds. Kinks are a new type of radiative-acoustic shock, and propagate at super-Abbottic speed.