TY  - JOUR
A1  - Hendrix, T.
A1  - Keppens, R.
T1  - Modelling colliding wind binaries in 2D
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-88198
SP  - 279
EP  - 282
ER  - 
TY  - JOUR
A1  - Groh, J. H.
T1  - The end stages of massive star evolution
BT  - WR stars as SN Ibc progenitors
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-88115
SP  - 237
EP  - 240
ER  - 
TY  - JOUR
A1  - Gull, T. R.
T1  - Eta Carinae
BT  - Many Advances .... Even More Puzzles
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-87876
SP  - 149
EP  - 154
ER  - 
TY  - JOUR
A1  - Meynet, G.
A1  - Georgy, C.
A1  - Maeder, A.
A1  - Ekström, S.
A1  - Groh, J. H.
A1  - Barblan, F.
A1  - Song, H. F.
A1  - Eggenberger, P.
T1  - Physics of massive stars relevant for the modeling of Wolf-Rayet populations
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-87971
SP  - 183
EP  - 188
ER  - 
TY  - JOUR
A1  - Morris, P. W.
T1  - Measuring η Carinae's High Mass Ejecta in the Infrared and Sub-millimeter
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-87895
SP  - 155
EP  - 158
ER  - 
TY  - JOUR
A1  - Vink, J. S.
T1  - The True origin of Wolf-Rayet stars
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-87848
SP  - 133
EP  - 138
ER  - 
TY  - JOUR
A1  - Madura, T. I.
A1  - Clementel, N.
A1  - Gull, T. R.
A1  - Kruip, C. J. H.
A1  - Paardekooper, J.-P.
A1  - Icke, V.
T1  - 3D hydrodynamical and radiative transfer modeling of η Carinae's colliding winds
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-87930
SP  - 163
EP  - 166
ER  - 
TY  - JOUR
A1  - Kourniotis, M.
A1  - Bonanos, A.
A1  - Najarro, F.
T1  - Accurate parameters of massive binaries in the Danks clusters
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-87819
SP  - 121
EP  - 124
ER  - 
TY  - JOUR
A1  - Liermann, A.
T1  - Evolution of Wolf-Rayet spectra
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-87830
SP  - 129
EP  - 132
ER  - 
TY  - JOUR
A1  - Koenigsberger, C.
T1  - HD5980
BT  - wind collisions and binary star evolution
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-87954
SP  - 171
EP  - 174
ER  - 
TY  - JOUR
A1  - Ramírez Alegría, S.
A1  - Chené, A.-N.
A1  - Borissova, J.
A1  - Kurtev, R.
A1  - Navarro, C.
A1  - Kuhn, M.
A1  - Carballo-Bello, J. A.
T1  - A not so massive cluster hosting a very massive star
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-88477
SP  - 362
ER  - 
TY  - JOUR
A1  - Ro, S.
A1  - Matzner, C. D.
T1  - Envelope Inflation or Stellar Wind?
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-88491
SP  - 364
ER  - 
TY  - JOUR
A1  - Beradze, S.
A1  - Kochiashvili, N.
A1  - Natsvlishvili, R.
A1  - Kochiashvili, I.
A1  - Janiashvili, E.
A1  - Urushadze, T.
A1  - Vardosanidze, M.
T1  - P Cygni and its Observations at the Abastumani Observatory
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-88389
SP  - 353
ER  - 
TY  - JOUR
A1  - Szécsi, D.
A1  - Langer, N.
A1  - Sanyal, D.
A1  - Evans, C. J.
A1  - Bestenlehner, J. M.
A1  - Raucq, F.
T1  - Do rapidly-rotating massive stars at low metallicity form Wolf–Rayet stars?
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-87997
SP  - 189
EP  - 192
ER  - 
TY  - GEN
A1  - Thiel, Marco
A1  - Romano, Maria Carmen
A1  - Kurths, Jürgen
A1  - Rolfs, Martin
T1  - Twin Surrogates to Test for Complex Synchronisation
N2  - We present an approach to generate (multivariate) twin surrogates (TS) based on recurrence properties. This technique generates surrogates which correspond to an independent copy of the underlying system, i. e. they induce a trajectory of the underlying system starting at different initial conditions. We show that these surrogates are well suited to test for complex synchronisation and exemplify this for the paradigmatic system of R¨ossler oscillators. The proposed test enables to assess the statistical relevance of a synchronisation analysis from passive experiments which are typical in natural systems.
T3  - Zweitveröffentlichungen der Universität Potsdam : Humanwissenschaftliche Reihe - paper 264 
Y1  - 2006
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-57231
ER  - 
TY  - JOUR
A1  - Reyes-Iturbide, J.
A1  - Velázquez, Pablo F.
A1  - Rosado, M.
T1  - 3D numerical model for NGC 6888 Nebula
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-88485
SP  - 363
ER  - 
TY  - JOUR
A1  - Toalá, Jesús Alberto
A1  - Guerrero, Martín A.
A1  - Chu, Y.-H.
A1  - Arthur, S. J.
A1  - Gruendl, R. A.
T1  - Diffuse X-ray Emission within Wolf-Rayet Nebulae
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-88316
SP  - 333
EP  - 336
ER  - 
TY  - JOUR
A1  - Guerrero, Martín A.
T1  - Planetary nebulae and Their Central Stars in X-rays
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-88160
SP  - 263
EP  - 266
ER  - 
TY  - JOUR
A1  - Gómez-González, Víctor Mauricio Alfonso
A1  - Mayya, Yalia Divakara
A1  - Rosa-González, D.
T1  - Detection and Characterization of Wolf-Rayet stars in M81 with GTC/OSIRIS spectra and HST images
JF  - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015
N2  - 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.
Y1  - 2015
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-87604
SP  - 43
EP  - 46
ER  - 
TY  - THES
A1  - Inal, Sahika
T1  - Responsive polymers for optical sensing applications
T1  - Responsive Polymere für optische Sensoren
N2  - LCST-type synthetic thermoresponsive polymers can reversibly respond to certain stimuli in aqueous media with a massive change of their physical state. When fluorophores, that are sensitive to such changes, are incorporated into the polymeric structure, the response can be translated into a fluorescence signal. Based on this idea, this thesis presents sensing schemes which transduce the stimuli-induced variations in the solubility of polymer chains with covalently-bound fluorophores into a well-detectable fluorescence output. Benefiting from the principles of different photophysical phenomena, i.e. of fluorescence resonance energy transfer and solvatochromism, such fluorescent copolymers enabled monitoring of stimuli such as the solution temperature and ionic strength, but also of association/disassociation mechanisms with other macromolecules or of biochemical binding events through remarkable changes in their fluorescence properties. For instance, an aqueous ratiometric dual sensor for temperature and salts was developed, relying on the delicate supramolecular assembly of a thermoresponsive copolymer with a thiophene-based conjugated polyelectrolyte. Alternatively, by taking advantage of the sensitivity of solvatochromic fluorophores, an increase in solution temperature or the presence of analytes was signaled as an enhancement of the fluorescence intensity. A simultaneous use of the sensitivity of chains towards the temperature and a specific antibody allowed monitoring of more complex phenomena such as competitive binding of analytes. The use of different thermoresponsive polymers, namely poly(N-isopropylacrylamide) and poly(meth)acrylates bearing oligo(ethylene glycol) side chains, revealed that the responsive polymers differed widely in their ability to perform a particular sensing function. In order to address questions regarding the impact of the chemical structure of the host polymer on the sensing performance, the macromolecular assembly behavior below and above the phase transition temperature was evaluated by a combination of fluorescence and light scattering methods. It was found that although the temperature-triggered changes in the macroscopic absorption characteristics were similar for these polymers, properties such as the degree of hydration or the extent of interchain aggregations differed substantially. Therefore, in addition to the demonstration of strategies for fluorescence-based sensing with thermoresponsive polymers, this work highlights the role of the chemical structure of the two popular thermoresponsive polymers on the fluorescence response. The results are fundamentally important for the rational choice of polymeric materials for a specific sensing strategy.
N2  - Als Reaktion auf bestimmte äußere Stimuli ändern bestimmte wasserlösliche Polymere reversibel ihren physikalischen Zustand. Dieser Vorgang kann mithilfe von Fluorophoren, die in die Polymerstrukturen eingebaut werden und deren Fluoreszenzeigenschaften vom Polymer¬zustand abhängen, detektiert werden. Diese Idee ist der Ausgangspunkt der vorliegenden Arbeit, die sich damit beschäftigt, wie äußerlich induzierte Änderungen der Löslichkeit solcher Polymere mit kovalent gebundenen Fluorophoren in Wasser in ein deutlich messbares Fluoreszenzsignal übersetzt werden können. Dazu werden photophysikalische Phänomene wie Fluoreszenz-Resonanz¬energie¬transfer und Solvatochromie ausgenutzt. In Kombination mit einem responsiven Polymergerüst wird es möglich, verschiedene Stimuli wie Lösungs¬temperatur oder Ionenstärke, oder auch Assoziation-Dissoziation Reaktionen mit anderen Makromolekülen oder biochemische Bindungs¬reaktionen über die Änderung von Fluorezenz¬farbe bzw. –Intensität autonom mit bloßem Auge zu detektieren. Unter anderem wurde ein wässriger ratiometrischer Temperatur- und Salzsensor entwickelt, der auf der komplexen supramolekularen Struktur eines thermoresponsiven Copolymers und eines thiophenbasierten konjugierten Polyelektrolyts beruht. Die Anbindung solvato¬chromer Fluorophore erlaubte den empfindlichen Nachweis einer Temperatur¬änderung oder des Vorhandenseins von Analyten. Komplexere Phänomene wie das kompetitive Anbinden von Analyten ließen sich hochempfindlich steuern und auslesen, indem gleichzeitig die Sensitivität dieser Polymeren gegenüber der Temperatur und spezifischen Antikörpern ausgenutzt wurde. Überraschenderweise wiesen die hier untersuchten thermoresponsiven Polymere wie poly-N-isopropylacrylamid (pNIPAm) oder poly-Oligoethylenglykolmethacrylate (pOEGMA) große Unterschiede bzgl. ihrer responsiven optischen Eigenschaften auf. Dies erforderte eine ausführliche Charakterisierung des Fluoreszenz- und Aggregationsverhaltens, unter- und oberhalb des Phasenübergangs, im Bezug auf die chemische Struktur. Ein Ergebnis war, dass alle drei Polymertypen sehr ähnliche temperaturabhängige makroskopische Absorptionseigenschaften aufweisen, während sich die Eigenschaften auf molekularer Ebene, wie der Hydratisierungsgrad oder die intermolekulare Polymerkettenaggregation, bei diesen Polymeren sehr unterschiedlich. Diese Arbeit zeigt damit anhand zweier sehr etablierter thermoresponsiver Polymere, nämlich pNIPAm und pOEGMA, das die chemische Struktur entscheidend für den Einsatz dieser Polymere in fluoreszenzbasierten Sensoren ist. Diese Ergebnisse haben große Bedeutung für die gezielte Entwicklung von Polymermaterialien für fluoreszenzbasierte Assays.
KW  - Responsive Polymere
KW  - Fluoreszenz
KW  - Sensor
KW  - Konjugierten polyelektrolyt
KW  - responsive polymer
KW  - fluorescence
KW  - sensor
KW  - conjugated polyelectrolyte
Y1  - 2013
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-70806
ER  -