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Carbon-rich Wolf-Rayet stars are efficient carbon dust makers. Despite the strong evidence for dust formation in these objects provided by infrared thermal emission from dust, the routes to nucleation and condensation and the physical conditions required for dust production are still poorly understood. We discuss here the potential routes to carbon dust and the possible locations conducive to dust formation in the colliding winds of WC binaries.
Observations of the WC9+OB system WR65 in the infrared show variations of its dust emission consistent with a period near 4.8 yr, suggesting formation in a colliding-wind binary (CWB) having an elliptical orbit. If we adopt the IR maximum as zero phase, the times of X-ray maximum count and minimum extinction to the hard component measured by Oskinova & Hamann fall at phases 0.4–0.5, when the separation of the WC9 and OB stars is greatest. We consider WR65 in the context of other WC8–9+OB stars showing dust emission.
WR Time Series Photometry
(2015)
We take a comprehensive look at Wolf Rayet photometric variability using the MOST satellite. This sample, consisting of 6 WR stars and 6 WC stars defies all typical photometric analysis. We do, however, confirm the presence of unusual periodic signals resembling sawtooth waves which are present in 11 out of 12 stars in this sample.
The stellar Eddington limit
(2015)
It is often assumed that when stars reach their Eddington limit, strong outflows are initiated, and that this happens only for extreme stellar masses. We discuss here that in models of up to 500 M⊙, the Eddington limit is never reached at the stellar surface. Instead, we argue that the Eddington limit is reached inside the stellar envelope in hydrogen-rich stars above ∼ 30 M⊙ and in Wolf-Rayet stars above ∼ 7 M⊙, with drastic effects for their struture and stability.
We look at how the dynamics of colliding wind binaries (CWB) can be investigated in 2D, and how several parameters influence the dynamics of the small scale structures inside the colliding wind and the shocked regions, as well as in how the dynamics influence the shape of the collision region at large distances. The parameters we adopt are based on the binary system WR98a, one of the few Wolf-Rayet (WR) dusty pinwheels known.
The morphological appearance of massive stars across their post-Main Sequence evolution and before the SN event is very uncertain, both from a theoretical and observational perspective. We recently developed coupled stellar evolution and atmospheric modeling of stars done with the Geneva and CMFGEN codes, for initial masses between 9 and 120 M⊙. We are able to predict the observables such as the high-resolution spectrum and broadband photometry. Here I discuss how the spectrum of a massive star changes across its evolution and before death, with focus on the WR stage. Our models indicate that single stars with initial masses larger than 30 M⊙ end their lives as WR stars. Depending on rotation, the spectrum of the star can either be that of a WN or WO subtype at the pre-SN stage. Our models allow, for the first time, direct comparison between predictions from stellar evolution models and observations of SN progenitors.
Eta Carinae
(2015)
Since Augusto Damineli's demonstration in 1996 that Eta Carinae is a binary with a 5.52 year period, many innovative observations and increasingly advanced three-dimensional models have led to considerable insight on this massive system that ejected at least ten, possibly forty, solar masses in the nineteenth century. Here we present a review of our current understanding of this complex system and point out continuing puzzles.
Key physical ingredients governing the evolution of massive stars are mass losses, convection and mixing in radiative zones. These effects are important both in the frame of single and close binary evolution. The present paper addresses two points: 1) the differences between two families of rotating models, i.e. the family of models computed with and without an efficient transport of angular momentum in radiative zones; 2) The impact of the mass losses in single and in close binary models.
I address uncertainties on the spatial distribution and mass of the dust formed in η Carinae's Homunculus nebula with data being combined from several space- and ground-based facilities spanning near-infrared to sub-mm wavelengths, in terms of observational constraints and modeling. Until these aspects are better understood, the mass loss history and mechanisms responsible for η Car's enormous eruption(s) remain poorly constrained.
The Wolf-Rayet (WR) phenomenon is widespread in astronomy. It involves classical WRs, very massive stars (VMS), WR central stars of planetary nebula CSPN [WRs], and supernovae (SNe). But what is the root cause for a certain type of object to turn into an emission-line star? In this contribution, I discuss the basic aspects of radiation-driven winds that might reveal the ultimate difference between WR stars and canonical O-type stars. I discuss the aspects of (i) self-enrichment via CNO elements, (ii) high effective temperatures (Tₑff), (iii) an increase in the helium abundance (Y ), and finally (iv) the Eddington factor Γₑ. Over the last couple of years, we have made a breakthrough in our understanding of Γₑ -dependent mass loss, which will have far-reaching consequences for the evolution and fate of the most massive stars in the Universe. Finally, I discuss the prospects for studies of the WR phenomenon in the highest redshift Lyα and He ii emitting galaxies.
We present results of full 3D hydrodynamical and radiative transfer simulations of the colliding stellar winds in the massive binary system η Carinae. We accomplish this by applying the SimpleX algorithm for 3D radiative transfer on an unstructured Voronoi-Delaunay grid to recent 3D smoothed particle hydrodynamics (SPH) simulations of the binary colliding winds. We use SimpleX to obtain detailed ionization fractions of hydrogen and helium, in 3D, at the resolution of the original SPH simulations. We investigate several computational domain sizes and Luminous Blue Variable primary star mass-loss rates. We furthermore present new methods of visualizing and interacting with output from complex 3D numerical simulations, including 3D interactive graphics and 3D printing. While we initially focus on η Car, the methods employed can be applied to numerous other colliding wind (WR 140, WR 137, WR 19) and dusty `pinwheel' (WR 104, WR 98a) binary systems. Coupled with 3D hydrodynamical simulations, SimpleX simulations have the potential to help determine the regions where various observed time-variable emission and absorption lines form in these unique objects.
We present results from our near-infrared spectroscopy with VLT/ISAAC of four, massive eclipsing binary systems in the young, heavily reddened, massive Danks clusters. We derive accurate fundamental parameters and the distance to these massive systems, which comprise of OIf+, WR and O-type stars. Our goal is to increase the sample of well-studied WR stars and constrain their physics by comparison with evolutionary models.
Wolf-Rayet stars are important sources for the enrichment of the ISM with nuclear processed elements, UV photons and momentum. They are descendants of high-mass stars for which short lifetimes and transition times can hamper the spectral classification of the stars in their different evolutionary phases. The expanded stellar atmospheres of Wolf-Rayet stars can show spectra which seem inconsistent with the anticipated underlying evolution phase, for example in late hydrogen-burning WN stars and Of/WN transition stars. We present a sequence of synthetic spectra of the Potsdam Wolf-Rayet models based on the latest Geneva stellar evolution models. This will visualize the changes in stellar spectra over a full stellar lifetime. Direct comparison with observed stellar spectra, as well as the evolution of diagnostic line ratios will improve the connection of spectral classification and evolution phase.
HD5980
(2015)
HD5980 is a multiple system containing at least 3 very massive and luminous stars. Located in the Small Magellanic Cloud, it is an ideal system for studying the massive star structure and evolutionary processes in low-metallicity environments. Intensely observed over the past few decades, HD5980 is a treasure trove of information on stellar wind structure, on wind-wind collisions and on the formation of wind-blown circumstellar structures. In addition, its characteristics suggest that the eclipsing WR+LBV stars of the system are the product of quasihomogeneous chemical evolution, thus making them candidate pair production supernovae or GRB progenitors. This paper summarizes some of the outstanding results derived from half a century of observations and recent theoretical studies.
We present the first physical characterization of the young open cluster VVVCL041. We spectroscopically observed the cluster main-sequence stellar population and a very-massive star candidate: WR62-2. CMFGEN modelling to our near-infrared spectra indicates that WR62-2 is a very luminous (10^6.4±0.2 L⊙)and massive (∼ 80M⊙) star.
We an optically-thick, transonic, steady wind model for a H-free Wolf-Rayet star. A bifurcation is found across a critical mass loss rate Mb. Slower winds M < Mb extend by several hydrostatic stellar radii, reproduce features of envelope in ation from Petrovic et al. (2006) and Gräfener et al. (2012), and are energetically unbound. This work is of particular interest for extended envelopes and winds, radiative hydrodynamic instabilities (eg. wind stagnation, clumping, etc.), and NLTE atmospheric models.
We found original observations of PCygni by E. Kharadze and N. Magalashvili in the archives of the Abastumani Observatory. These observations were carried out in the period 1951–1983. Initially they used 29 Cygni as a comparison star, and all observations of PCygni were processed using this star. On the basis of their calculations, the authors decided that PCygni may be a WUMa type binary with an orbital period of 0.500565 d, but this hypothesis was not confirmed. The only observations that have been published in the Bulletin of the Abastumani Astrophysical Observatory were those of of 1951–1955. There are whole sets of observational data not only for PCygni and 29 Cygni, but in the majority of cases also for 36 Cygni in the archives. We recalculated all data (where it was possible) using 36 Cygni as a comparison star. We are presenting UBV light curves of the variable, and also observations made by V. Nikonov in Abastumani in the period 1935–1937
Die Arbeitswelt im Fokus
(2015)
Für Bachelor-Studierende der Wirtschaftsinformatik im zweiten Semester an der Fachhochschule Kiel werden im Modul Informationsmanagement neben klassischen didaktischen Ansätzen in einer seminaristischen Unterrichtsform so genannte „Aktivbausteine“ eingesetzt: Studierende erhalten zum einen die Gelegenheit, sich im Kontakt mit Fach- und Führungskräften aus der Industrie ein konkretes Bild vom Beruf der Wirtschaftsinformatikerin bzw. des Wirtschaftsinformatikers zu machen; zum anderen erarbeiten sie innovative Ansätze der Prozessverbesserung aus Sicht der IT oder mit Nutzenpotenzial für die IT und präsentieren ihre Ergebnisse öffentlich im Rahmen des Kieler Prozessmanagementforums. Diese Aktivbausteine dienen insbesondere der Berufsfeldorientierung: Durch die Informationen, die die Studierenden über die Anforderungen und Tätigkeiten von im Beruf stehenden Menschen erhalten, werden sie in die Lage versetzt, fundierte Entscheidungen bzgl. ihrer Studiengestaltung und Berufswahl zu treffen. Im Beitrag wird die Konzeption der Bausteine vorgestellt und deren Grad der Zielerreichung durch aktuelle Evaluationsergebnisse erläutert. Zudem wird die motivationale Wirkung der Aktivbausteine anhand der Theorie der Selbstbestimmung von Deci und Ryan [DR1985, DR1993, DR2004] erläutert.
The evolution of massive stars is strongly influenced by their initial chemical composition. We have computed rapidly-rotating massive star models with low metallicity (∼1/50 Z⊙) that evolve chemically homogeneously and have optically-thin winds during the main sequence evolution. These luminous and hot stars are predicted to emit intense mid- and far-UV radiation, but without the broad emission lines that characterize WR stars with optically-thick winds. We show that such Transparent Wind UV-Intense (TWUIN) stars may be responsible for the high number of He ii ionizing photons observed in metal-poor dwarf galaxies, such as IZw 18. We find that these TWUIN stars are possible long-duration gamma-ray burst progenitors.
In 1945, Zinovii Shenderovich Tolkatchev (1903–1977), a Soviet artist of Jewish origin, created a striking series of five images entitled “Jesus in Majdanek”. The series was the culmination of Tolkatchev‘s intensive preoccupation with the experience he, as a Red Army soldier, endured upon taking part in liberation of the concentration camps Majdanek and Auschwitz. Shocked by the actual sights he witnessed, he depicted Jesus as an actual camp inmate, wearing a striped uniform marked by every possible defamation sign – the Jewish yellow star, the red triangle of political prisoners, and the individual prison number, the numerical tattoo on his lower arm can also be seen. The different stages of camp life are portrayed as the traditional Passion of Christ. While showing the actual situations the artist based himself upon the well known European Renaissance paintings canonically depicting Jesus‘ suffering. The article places Tolkatchev‘s series in a broader cultural and visual context by exploring the development of the ‘historical Jesus’ in the 19th century European thought and Russian realist art, and by examining the impact of the German avant-garde. By doing so, a deeper understanding of the universal message Tolkatchev’s works entail is offered.
Messianic Jews are Jewish individuals who syncretically accept both the messianic character of Jesus and the ritual cultic practices provided by traditional Judaism. The present article examines the emergence of this marginal syncretic movement in contemporary Israel, and maintains that it represents a radical development in the bimillenary history of Jewish-Christian relations. This article offers a general introduction to the notion of Jewish-Christian identity, a brief history of the first group of Messianic Jews in the Land of Israel, the cultural influence and religious syncretism of the Messianic Jews in modern Israel, and, finally, the implication that Messianic Judaism is supposed to become the new paradigm within the various branches of Judaism.
Bereits in der aufklärerischen Auseinandersetzung um Jesus’ Judentum finden sich Tendenzen, dieses als Ausgangspunkt einer universalisierenden Vermittlung zwischen Judentum und Christentum zu entwerfen, wie auch – zumeist von jüdischer Seite – Einsprüche gegen einen derartigen Universalismus, der entscheidende Differenzen und die Geschichte ausgrenzender Gewalt verleugne. Nach einem kurzen Blick auf den jüdischen Christus bei Heine analysiert der Beitrag Stefan Zweigs im Horizont des Ersten Weltkriegs und zionistischer Debatten entstandenes, 1917 publiziertes Drama „Jeremias“. Die für die Konzeption des Stückes zentrale Überblendung der Prophetenfigur Jeremias mit Christus treibt, so die These, die problematische Logik einer Opferstellvertretung hervor, die mit der Vorstellung einer durch (Opfer-)Blut konstituierten Gemeinschaft die Frage nach der Schuld (Christusmord) auf Andere verschiebt. Demgegenüber entwirft das Stück in Motiven der einbrechenden ‚Schrecknis‘, der Fremdheit im Eigenen, des Exils und der Weltwanderschaft einen anderen Kosmopolitismus.
Der deutsch-jüdische Dichter und Anarchist Erich Mühsam (1878–1934) rekurrierte in seinem schriftstellerischen OEuvre wiederholt auf die Figur Jesus’. Im Versuch, diese Beziehungsgeschichte zu rekonstruieren und zu deuten, rücken Einflussgeber aus dem Umfeld der literarischen Avantgarde Berlins sowie der Lebensreformbewegung in den Blick. In einer Verschränkung von quasireligiöser Renaissance und Aufbruchstimmung hin zum ‚Neuen Menschen‘ war Jesus in diesen Zirkeln um die Jahrhundertwende ein beliebtes Motiv und prägte sich, vermittelt über Freundschaften und Wegmarken, auch in Mühsams Schreiben ein. Neben Kain ist es Jesus, der bei Mühsam zur den fünften Stand revolutionierenden Lichtgestalt wird. In diese Bezugnahme spielen Mühsams konfliktreiches Verhältnis zu seinem Vater und dessen Assimilation an das deutsche Bürgertum mit hinein, das keineswegs gänzlich jene aufgeklärten Werte lebte, auf die es sich nominell berief: Statt Freiheit und Gleichheit prävalierten neue Zwänge, Begrenzungen und Ressentiments, wie Mühsam bemerkte. Über Gustav Landauer fand er nicht nur zum Anarchismus, sondern auch zu einer neuen Sprache für die verschüttete Tradition und prägte hierüber seiner Jesusfigur sein Verständnis eines rebellischen Judentums ein, das Mühsam selbst als Revolutionär verkörperte.
Jakob Wassermanns Roman „Die Juden von Zirndorf“ (1897), ein Sittengemälde deutsch-jüdischen Lebens, ist von diversen messianischen Vorstellungen getragen, die nur zum Teil auf die jüdische Tradition zurückzuführen sind. Folglich vereint der jüdische Knabe Agathon, die Hauptgestalt des zweiten Romanteils, Züge sowohl des jüdischen Messias als auch des christlichen Heilands. Die hohe Anzahl von Anspielungen auf die Figur Jesu und die ästhetische Funktionalisierung christologischer Motive im Roman ist in den Kontext jener „Heimholung Jesu in das Judentum“ einzubetten, die ab dem 19. Jahrhundert mit der Wissenschaft des Judentums einsetzte. Der vorliegende Beitrag wird – vor dem Hintergrund zeitgenössischer Jesus-Deutungen – sowohl auf die Spuren Jesu in der Charakterisierung Agathons als auch auf die Aneignung christologischer Motive vor allem im 2. Romanteil eingehen. Dabei soll insbesondere auf Lou von Salomés Aufsatz „Jesus der Jude“ (1896) als mögliche Quelle verwiesen werden.
Die jüdischen Künstler Maurycy Gottlieb (1856–1879) und Marc Chagall (1887–1985) stellten Jesus als gläubigen Juden, eingebettet in die jüdische Umwelt seiner Zeit, dar. Der jüdische Jesus wird für sie zu einer Auseinandersetzung mit den jüdischen Wurzeln des Christentums und mit dem Antisemitismus, und sein Martyrium zu einem Symbol des jüdischen Leidens. Der vorliegende Aufsatz untersucht, wie ihre Bilder diese Botschaften transportieren und analysiert Kontinuitäten und Brüche über einen langen Zeitraum hinweg.
Carl Einsteins Drama „Die schlimme Botschaft“ (1921), das ihm einen Prozess wegen Gotteslästerung einbrachte, steht mit seiner kritischen Haltung gegenüber der christlichen Lehre von der Kreuzigung und Auferstehung im Trend einer seinerzeit von jüdischen Theologen geführten Diskussion mit Adolf Harnacks Modernisierungsprojekt des Christentums. Jüdische Theologen wie Joseph Eschelbacher entwarfen ein Judentum, das, anders als von Harnack dargestellt, bereits jene moderne Gestalt einer Religion erfüllt, die Harnack für das Christentum erst zu erreichen versuchte. Einsteins „vom Dogma abweichende[r] Standpunkt“, der ihm vor Gericht von einem katholischen Geistlichen als Standpunkt eines dissidenten Juden vorgeworfen wurde, hätte durchaus als Beitrag eines jüdischen Literaten zur Apologie des Judentums gelten können, wenn Einstein nicht selbst seine Glaubensbrüder im Verbund mit der von ihm abgelehnten bürgerlichen Ideologie des kapitalistischen Marktes gesehen hätte.
E-Learning
(2015)
For the calculation of the work in an irreversible pressure-volume change, we propose approxima-tions, which in contrast to the usual representation in the literature reflect the work performed during expansion and compression symmetrically. The calculations are based on the Reversible-Share-Theorem: Is used the force to overcome for calculating the work, so it captures only the configurational reversible work share.
When Jesus Spoke Yiddish
(2015)
In this paper, I wish to bring some evidences from a Yiddish manuscript of the “Toledot Yeshu” which has not yet been the object of research: MS. Günzburg, 1730 kept in the Russian State Library in Moscow and dated 17th century. The manuscript is part of the so-called ‘Herode-tradition’ of the “Toledot Yeshu”. This means that the Yiddish manuscript is connected to the version printed in Hebrew and accompanied by a Latin translation by the Swiss pastor and theologian Johann Jacob Uldrich (Huldricus, 1683–1731) in Leiden in 1705, bearing the title “Historia Jeschuae Nazareni”. Given the uncertainty about the exact dating of the Yiddish manuscript, a comparison between the Hebrew and the Yiddish can still allow some remarks concerning the characteristics of the Yiddish version and posit some questions about the transmission and the reception of this challenging and intriguing text.
In diesem Beitrag soll es darum gehen, anhand der Distinktion von Jetztzeit und Erinnerung scheinbare Einheiten im lyrischen Werk der Nelly Sachs zu hinterfragen. Ein Nexus der Jesusfigur zur Shoah ist in den Gedichten nicht zu übersehen; inwieweit eine Korrelation beider Diskurse zwischen dem perennierenden Leiden der Opfer und dem am Kreuz Gemarterten besteht, ist der Gegenstand dieser Untersuchung. Jesus wird im lyrischen Oeuvre auf der zeitlichen wie inhaltlichen Ebene neu figuriert: nicht als christologisch-dogmatische Erlöserfigur, sondern als der qualvoll gemarterte Mann, dessen Schrei im 20. Jahrhundert eine neue Lesbarkeit generiert: als leidender Mit-Bruder. Der historische Index der Jesus-Gestalt wird in der Passionsszenerie, die jedoch transformativ modifiziert wird, manifest.
We present 3D numerical simulations of the NGC6888 nebula considering the proper motion and the evolution of the star, from the red supergiant (RSG) to the Wolf-Rayet (WR) phase. Our simulations reproduce the limb-brightened morphology observed in [OIII] and X-ray emission maps. The synthetic maps computed by the numerical simulations show filamentary and clumpy structures produced by instabilities triggered in the interaction between the WR wind and the RSG shell.
We discuss our most recent findings on the diffuse X-ray emission within Wolf-Rayet (WR) nebulae. The best-quality X-ray observations of these objects are those performed by XMM- Newton and Chandra towards S 308, NGC 2359, and NGC 6888. Even though these three WR nebulae might have different formation scenarios, they all share similar characteristics: i) the main plasma temperatures of the X-ray-emitting gas is found to be T =[1–2]×^K, ii) the diffuse X-ray emission is confined inside the [O iii] shell, and iii) their X-ray luminosities and electron densities in the 0.3–2.0 keV energy range are LX ≈10^33–10^34 erg s-1 and ne ≈0.1–1 cm^-3 . These properties and the nebular-like abundances of the hot gas suggest mixing and/or thermal conduction is taking an important rôle reducing the temperature of the hot bubble.
Two types of X-ray sources are mostly found in planetary nebulae (PNe): point sources at their central stars and diffuse emission inside hot bubbles. Here we describe these two types of sources based on the most recent observations obtained in the framework of the Chandra Planetary Nebula Survey, ChanPlaNS, an X-ray survey targeting a volume-limited sample of PNe. Diffuse X-ray emission is found preferentially in young PNe with sharp, closed inner
shells. Point sources of X-ray emission at the central stars reveal magnetically active binary companions and shock-in stellar winds.
Detection and Characterization of Wolf-Rayet stars in M81 with GTC/OSIRIS spectra and HST images
(2015)
Here we investigate a sample of young star clusters (YSCs) and other regions of recent star formation with Wolf-Rayet (W-R) features detected in the relatively nearby spiral galaxy M81 by analysing long-slit (LS) and Multi-Object Spectroscopy (MOS) spectra obtained with the OSIRIS instrument at the 10.4-m Gran Telescopio Canarias (GTC). We take advantage of the synergy between GTC spectra and Hubble Space Telescope (HST) images to also reveal their spatial localization and the environments hosting these stars. We finally discuss and comment on the next steps of our study.
forum:logopädie 29.2015, 5
(2015)
forum:logopädie 29.2015, 3
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forum:logopädie 29.2015, 1
(2015)
forum:logopädie 29.2015, 6
(2015)
forum:logopädie 29.2015, 4
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forum:logopädie 29.2015, 2
(2015)
Wolf-Rayet (WR) stars lose copious amounts of mass and momentum through dense stellar winds. The interaction of these outflows with their surroundings results in highly structured and complex circumstellar environments, often featuring knots, arcs, shells and spirals. Recent improvements in computational power and techniques have led to the development of detailed, multi-dimensional simulations that have given new insight into the origin of these structures, and better understanding of the physical mechanisms driving their formation. We review three of the main mechanisms that shape the outflows of WR stars:
• interaction with the interstellar medium (ISM), i.e., wind-ISM interactions;
• interaction with a stellar wind, either from a previous phase of evolution or the wind from a companion star, i.e., wind-wind interactions;
• and interaction with a companion star that has a weak or insignificant outflow (e.g., a compact companion such as a neutron star or black hole), i.e.,wind-companion interactions.
We also highlight the broader implications and impact of these circumstellar structures for related phenomena, e.g., for X-ray binaries and Gamma-ray bursts.