@inproceedings{DaviesVinkOudmaijer2007,
  author    = {Davies, B. and Vink, J. S. and Oudmaijer, R. D.},
  title     = {Modelling the polarimetric variability of hot stars},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17939},
  year      = {2007},
  abstract  = {Many hot stars exhibit stochastic polarimetric variability, thought to arise from clumping low in the wind. Here we investigate the wind properties required to reproduce this variability using analytic models, with particular emphasis on Luminous Blue Variables. We find that the winds must be highly structured, consisting of a large number of optically-thin clumps; while we find that the overall level of polarization should scale with mass-loss rate - consistent with observations of LBVs. The models also predict variability on very short timescales, which is supported by the results of a recent polarimetric monitoring campaign.},
  language  = {en}
}
@inproceedings{KubatSaad2007,
  author    = {Kub{\´a}t, Jiř{\´i} and Saad, S. M.},
  title     = {Moving absorption bumps in the spectra of Be stars},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17879},
  year      = {2007},
  abstract  = {Several Be binaries exhibit an absorption bump moving across the blue wing of hydrogen emission lines towards the line center. This bump is demonstrated for the case of two bright Be stars, κ Dra and 4 Her. It is not clear what is the reason for this travelling bump.},
  language  = {en}
}
@inproceedings{Nielsen2007,
  author    = {Nielsen, K. E.},
  title     = {On irregular line profiles in the optical spectrum of Eta Carinae},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18227},
  year      = {2007},
  abstract  = {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.},
  language  = {en}
}
@inproceedings{CohenLeuteneggerTownsend2007,
  author    = {Cohen, David H. and Leutenegger, M. A. and Townsend, R. H. D.},
  title     = {Quantitative analysis of resolved X-ray emission line profiles of O stars},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18115},
  year      = {2007},
  abstract  = {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.},
  language  = {en}
}
@inproceedings{MorrisonRotherKurschat2007,
  author    = {Morrison, N. D. and Rother, R. and Kurschat, N.},
  title     = {Hα line profile variability in the B8Ia-type supergiant Rigel (β Ori)},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18120},
  year      = {2007},
  abstract  = {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.},
  language  = {en}
}
@inproceedings{CheneMoffatCrowther2007,
  author    = {Chen{\´e}, A.-N. and Moffat, Anthony F. J. and Crowther, P. A.},
  title     = {Rapidly accelerating clumps in the winds of the very hot WNE Stars},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18163},
  year      = {2007},
  abstract  = {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.},
  language  = {en}
}
@inproceedings{Kholtygin2007,
  author    = {Kholtygin, A. F.},
  title     = {Modelling the induced clumping stochastic line profile variability},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18180},
  year      = {2007},
  abstract  = {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.},
  language  = {en}
}
@inproceedings{Cassinelli2007,
  author    = {Cassinelli, Joseph P.},
  title     = {Discussion: Magnetic fields, variability},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18195},
  year      = {2007},
  language  = {en}
}
@inproceedings{StLouis2007,
  author    = {St-Louis, N.},
  title     = {Discussion: Binaries, colliding winds, LBVs and high energy radiation},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18155},
  year      = {2007},
  abstract  = {Clumping in hot-star winds : proceedings of an international workshop held in Potsdam, Germany, 18. - 22. June 2007},
  language  = {en}
}
@misc{FreseGarstFay2007,
  author    = {Frese, Michael and Garst, Harry and Fay, Doris},
  title     = {Making things happen : reciprocal relationships between work characteristics and personal initiative in a four-wave longitudinal structural equation model},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18278},
  year      = {2007},
  abstract  = {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.},
  language  = {en}
}
@misc{FayGuillaume2007,
  author    = {Fay, Doris and Guillaume, Yves R. F.},
  title     = {Team diversity},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18295},
  year      = {2007},
  abstract  = {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.},
  language  = {en}
}
@inproceedings{RomeroOwockiAraudoetal.2007,
  author    = {Romero, G. E. and Owocki, S. P. and Araudo, A. T. and Townsend, R. H. D. and Benaglia, P.},
  title     = {Using gamma-rays to probe the clumped structure of stellar winds},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18210},
  year      = {2007},
  abstract  = {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.},
  language  = {en}
}
@inproceedings{Weis2007,
  author    = {Weis, K.},
  title     = {Wind relics : clumps, inhomogeneities and outflows in LBV nebulae},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18235},
  year      = {2007},
  abstract  = {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.},
  language  = {en}
}
@misc{WackervonElert2001,
  author    = {Wacker, Alexander and von Elert, Eric},
  title     = {Polyunsaturated fatty acids : evidence for non-substitutable biochemical resources in Daphnia galeata},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17587},
  year      = {2001},
  abstract  = {The factors that determine the efficiency of energy transfer in aquatic food webs have been investigated for many decades. The plant-animal interface is the most variable and least predictable of all levels in the food web. In order to study determinants of food quality in a large lake and to test the recently proposed central importance of the long-chained eicosapentaenoic acid (EPA) at the pelagic producer-grazer interface, we tested the importance of polyunsaturated fatty acids (PUFAs) at the pelagic producerconsumer interface by correlating sestonic food parameters with somatic growth rates of a clone of Daphnia galeata. Daphnia growth rates were obtained from standardized laboratory experiments spanning one season with Daphnia feeding on natural seston from Lake Constance, a large pre-alpine lake. Somatic growth rates were fitted to sestonic parameters by using a saturation function. A moderate amount of variation was explained when the model included the elemental parameters carbon (r2 = 0.6) and nitrogen (r2 = 0.71). A tighter fit was obtained when sestonic phosphorus was incorporated (r2 = 0.86). The nonlinear regression with EPA was relatively weak (r2 = 0.77), whereas the highest degree of variance was explained by three C18-PUFAs. The best (r2 = 0.95), and only significant, correlation of Daphnia's growth was found with the C18-PUFA α-linolenic acid (α-LA; C18:3n-3). This correlation was weakest in late August when C:P values increased to 300, suggesting that mineral and PUFA-limitation of Daphnia's growth changed seasonally. Sestonic phosphorus and some PUFAs showed not only tight correlations with growth, but also with sestonic α-LA content. We computed Monte Carlo simulations to test whether the observed effects of α-LA on growth could be accounted for by EPA, phosphorus, or one of the two C18-PUFAs, stearidonic acid (C18:4n-3) and linoleic acid (C18:2n-6). With >99 \% probability, the correlation of growth with α-LA could not be explained by any of these parameters. In order to test for EPA limitation of Daphnia's growth, in parallel with experiments on pure seston, growth was determined on seston supplemented with chemostat-grown, P-limited Stephanodiscus hantzschii, which is rich in EPA. Although supplementation increased the EPA content 80-800x, no significant changes in the nonlinear regression of the growth rates with α-LA were found, indicating that growth of Daphnia on pure seston was not EPA limited. This indicates that the two fatty acids, EPA and α-LA, were not mutually substitutable biochemical resources and points to different physiological functions of these two PUFAs. These results support the PUFA-limitation hypothesis for sestonic C:P < 300 but are contrary to the hypothesis of a general importance of EPA, since no evidence for EPA limitation was found. It is suggested that the resource ratios of EPA and α-LA rather than the absolute concentrations determine which of the two resources is limiting growth.},
  language  = {en}
}
@misc{WackervonElert2002,
  author    = {Wacker, Alexander and von Elert, Eric},
  title     = {Strong influences of larval diet history on subsequent post-settlement growth in the freshwater mollusc Dreissena polymorpha},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17627},
  year      = {2002},
  abstract  = {Significant seasonal variation in size at settlement has been observed in newly settled larvae of Dreissena polymorpha in Lake Constance. Diet quality, which varies temporally and spatially in freshwater habitats, has been suggested as a significant factor influencing life history and development of freshwater invertebrates. Accordingly, experiments were conducted with field-collected larvae to test the hypothesis that diet quality can determine planktonic larval growth rates, size at settlement and subsequent post-metamorphic growth rates. Larvae were fed one of two diets or starved. One diet was composed of cyanobacterial cells which are deficient in polyunsaturated fatty acids (PUFAs), and the other was a mixed diet rich in PUFAs. Freshly metamorphosed animals from the starvation treatment had a carbon content per individual 70\% lower than that of larvae fed the mixed diet. This apparent exhaustion of larval internal reserves resulted in a 50\% reduction of the postmetamorphic growth rates. Growth was also reduced in animals previously fed the cyanobacterial diet. Hence, low food quantity or low food quality during the larval stage of D. polymorpha lead to irreversible effects for postmetamorphic animals, and is related to inferior competitive abilities.},
  language  = {en}
}
@misc{SteinfathGaertnerLisecetal.2009,
  author    = {Steinfath, Matthias and G{\"a}rtner, Tanja and Lisec, Jan and Meyer, Rhonda C. and Altmann, Thomas and Willmitzer, Lothar and Selbig, Joachim},
  title     = {Prediction of hybrid biomass in Arabidopsis thaliana by selected parental SNP and metabolic markers},
  series = {Zweitver{\"o}ffentlichungen der Universit{\"a}t Potsdam : Mathematisch-Naturwissenschaftliche Reihe},
  journal   = {Zweitver{\"o}ffentlichungen der Universit{\"a}t Potsdam : Mathematisch-Naturwissenschaftliche Reihe},
  number    = {1324},
  issn      = {1866-8372},
  doi       = {10.25932/publishup-43111},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-431115},
  pages     = {9},
  year      = {2009},
  abstract  = {A recombinant inbred line (RIL) population, derived from two Arabidopsis thaliana accessions, and the corresponding testcrosses with these two original accessions were used for the development and validation of machine learning models to predict the biomass of hybrids. Genetic and metabolic information of the RILs served as predictors. Feature selection reduced the number of variables (genetic and metabolic markers) in the models by more than 80\% without impairing the predictive power. Thus, potential biomarkers have been revealed. Metabolites were shown to bear information on inherited macroscopic phenotypes. This proof of concept could be interesting for breeders. The example population exhibits substantial mid-parent biomass heterosis. The results of feature selection could therefore be used to shed light on the origin of heterosis. In this respect, mainly dominance effects were detected.},
  language  = {en}
}
@phdthesis{Scholz2012,
  author    = {Scholz, Markus Reiner},
  title     = {Spin polarization, circular dichroism, and robustness of topological surface states},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-96686},
  school      = {Universit{\"a}t Potsdam},
  pages     = {153},
  year      = {2012},
  abstract  = {Dreidimensionale topologische Isolatoren sind ein neues Materialsystem, welches dadurch charakterisiert ist, dass es in seinem Inneren isolierend an der Ober {\"a}che jedoch leitend ist. Urs{\"a}chlich f{\"u}r die Leitf{\"a}higkeit an der Ober {\"a}che sind sogenannte topologische Ober- {\"a}chenzust{\"a}nde, welche das Valenzband des Inneren mit dem Leitungsband des Inneren verbinden. An der Ober {\"a}che ist also die Bandl{\"u}cke, welche die isolierende Eigenschaft verursacht, geschlossen. Die vorliegende Arbeit untersucht diese Ober {\"a}chenzust{\"a}nde mittels spin- und winkelauf- gel{\"o}ster Photoemissionsspektroskopie. Es wird gezeigt, dass in den Materialien Bi2Se3 und Bi2Te3, in {\"u}bereinstimmung mit der Literatur, die entscheidenden Charakteristika eines topologischen Ober {\"a}chenzustands vorzu nden sind: Die Ober {\"a}chenzust{\"a}nde dieser Sys- teme durchqueren die Bandl{\"u}cke in ungerader Anzahl, sie sind nicht entartet und weisen folgerichtig eine hohe Spinpolarisation auf. Weiterhin wird durch Aufdampfen diverser Adsorbate gezeigt, dass der Ober {\"a}chenzust{\"a}n- de von Bi2Se3 und Bi2Te3, wie erwartet, extrem robust ist. Ober {\"a}chenzust{\"a}nde topologisch trivialer Systeme erf{\"u}llen diese Eigenschaft nicht; bereits kleine Verunreinigungen k{\"o}n- nen diese Zust{\"a}nde zerst{\"o}ren, bzw. die Ober {\"a}che isolierend machen. Die topologischen Ober {\"a}chenzust{\"a}nde k{\"o}nnen in der vorliegenden Arbeit noch bis zur Detektionsgrenze der experimentellen Messmethode nachgewiesen werden und die Ober {\"a}che bleibt Leitf{\"a}hig. Unter den Adsorbaten be ndet sich auch Eisen, ein bekanntermaßen magnetisches Materi- al. Eine der Grundvoraussetzungen f{\"u}r topologische Isolatoren ist die Zeitumkehrsymme- trie, die Elektronen, welche den topologischen Ober {\"a}chenzustand besetzen, vorschreibt, dass sie eine bestimmte Spinrichtung haben m{\"u}ssen, wenn sie sich beispielsweise nach links bewegen und den entgegengesetzten Spin wenn sie sich nach rechts bewegen. In magnetischen Materialien ist die Zeitumkehrsymmetrie jedoch explizit gebrochen und die gezeigte Robustheit des Ober {\"a}chenzustands gegen magnetische Materialien daher uner- wartet. Die Zeitumkehrsymmetrie sorgt auch daf{\"u}r, dass eine Streuung der Elektronen um 180°, beispielsweise an einem Gitterdefekt oder an einem Phonon strikt verboten ist. Bei einem solchen Streuprozess bleibt die Spinrichtung erhalten, da aber in der Gegenrichtung nur Zust{\"a}nde mit entgegengesetztem Spin vorhanden sind kann das Elektron nicht in diese Richtung gestreut werden. Dieses Prinzip wird anhand der Lebensdauer der durch Pho- toemission angeregten Zust{\"a}nde untersucht. Hierbei wird gezeigt, dass die Kopplung der Elektronen des Ober {\"a}chenzustands von Bi2Te3 an Phononen unerwartet hoch ist und dass sich eine Anisotropie in der Bandstruktur des Selbigen auch in den Lebensdauern der ange- regten Zust{\"a}nde widerspiegelt. Weiterhin wird gezeigt, dass sich die Ein {\"u}sse von magne- tischen und nicht-magnetischen Verunreinigungen auf die Lebensdauern stark voneinander unterscheiden. Im letzten Teil der vorliegenden Arbeit wird untersucht, ob eine Asymmetrie in der Inten- sit{\"a}tsverteilung der winkelaufgel{\"o}sten Photoemissionsspektren, bei Anregung mit zirku- lar polarisiertem Licht, in Bi2Te3 R{\"u}ckschl{\"u}sse auf die Spinpolarisation der Elektronen erlaubt. Bei Variation der Energie des eingestrahlten Lichts wird ein Vorzeichenwechsel der Asymmetrie beobachtet. Daraus l{\"a}sst sich schlussfolgern, dass die Asymmetrie keine R{\"u}ckschl{\"u}sse auf die Spinpolarisation erlaubt.},
  language  = {en}
}
@techreport{AmannRzepka2021,
  type      = {Working Paper},
  author    = {Amann, Erwin and Rzepka, Sylvi},
  title     = {The Effect of Goal-Setting Prompts in a Blended Learning Environment},
  series = {CEPA Discussion Papers},
  journal   = {CEPA Discussion Papers},
  number    = {25},
  issn      = {2628-653X},
  doi       = {10.25932/publishup-49347},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-493476},
  pages     = {22, vi},
  year      = {2021},
  abstract  = {We investigate how inviting students to set task-based goals affects usage of an online learning platform and course performance. We design and implement a randomized field experiment in a large mandatory economics course with blended learning elements. The low-cost treatment induces students to use the online learning system more often, more intensively, and to begin earlier with exam preparation. Treated students perform better in the course than the control group: they are 18.8\% (0.20 SD) more likely to pass the exam and earn 6.7\% (0.19 SD) more points on the exam. There is no evidence that treated students spend significantly more time, rather they tend to shift to more productive learning methods. The heterogeneity analysis suggests that higher treatment effects are associated with higher levels of behavioral bias but also with poor early course behavior.},
  language  = {en}
}
@phdthesis{DeAndradeQueiroz2023,
  author    = {De Andrade Queiroz, Anna Barbara},
  title     = {The Milky Way disks, bulge, and bar sub-populations},
  doi       = {10.25932/publishup-59061},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-590615},
  school      = {Universit{\"a}t Potsdam},
  pages     = {xii, 187},
  year      = {2023},
  abstract  = {In recent decades, astronomy has seen a boom in large-scale stellar surveys of the Galaxy. The detailed information obtained about millions of individual stars in the Milky Way is bringing us a step closer to answering one of the most outstanding questions in astrophysics: how do galaxies form and evolve? The Milky Way is the only galaxy where we can dissect many stars into their high-dimensional chemical composition and complete phase space, which analogously as fossil records can unveil the past history of the genesis of the Galaxy. The processes that lead to large structure formation, such as the Milky Way, are critical for constraining cosmological models; we call this line of study Galactic archaeology or near-field cosmology. At the core of this work, we present a collection of efforts to chemically and dynamically characterise the disks and bulge of our Galaxy. The results we present in this thesis have only been possible thanks to the advent of the Gaia astrometric satellite, which has revolutionised the field of Galactic archaeology by precisely measuring the positions, parallax distances and motions of more than a billion stars. Another, though not less important, breakthrough is the APOGEE survey, which has observed spectra in the near-infrared peering into the dusty regions of the Galaxy, allowing us to determine detailed chemical abundance patterns in hundreds of thousands of stars. To accurately depict the Milky Way structure, we use and develop the Bayesian isochrone fitting tool/code called StarHorse; this software can predict stellar distances, extinctions and ages by combining astrometry, photometry and spectroscopy based on stellar evolutionary models. The StarHorse code is pivotal to calculating distances where Gaia parallaxes alone cannot allow accurate estimates. We show that by combining Gaia, APOGEE, photometric surveys and using StarHorse, we can produce a chemical cartography of the Milky way disks from their outermost to innermost parts. Such a map is unprecedented in the inner Galaxy. It reveals a continuity of the bimodal chemical pattern previously detected in the solar neighbourhood, indicating two populations with distinct formation histories. Furthermore, the data reveals a chemical gradient within the thin disk where the content of 𝛼-process elements and metals is higher towards the centre. Focusing on a sample in the inner MW we confirm the extension of the chemical duality to the innermost regions of the Galaxy. We find stars with bar shape orbits to show both high- and low-𝛼 abundances, suggesting the bar formed by secular evolution trapping stars that already existed. By analysing the chemical orbital space of the inner Galactic regions, we disentangle the multiple populations that inhabit this complex region. We reveal the presence of the thin disk, thick disk, bar, and a counter-rotating population, which resembles the outcome of a perturbed proto-Galactic disk. Our study also finds that the inner Galaxy holds a high quantity of super metal-rich stars up to three times solar suggesting it is a possible repository of old super-metal-rich stars found in the solar neighbourhood. We also enter into the complicated task of deriving individual stellar ages. With StarHorse, we calculate the ages of main-sequence turn-off and sub-giant stars for several public spectroscopic surveys. We validate our results by investigating linear relations between chemical abundances and time since the 𝛼 and neutron capture elements are sensitive to age as a reflection of the different enrichment timescales of these elements. For further study of the disks in the solar neighbourhood, we use an unsupervised machine learning algorithm to delineate a multidimensional separation of chrono-chemical stellar groups revealing the chemical thick disk, the thin disk, and young 𝛼-rich stars. The thick disk is shown to have a small age dispersion indicating its fast formation contrary to the thin disk that spans a wide range of ages. With groundbreaking data, this thesis encloses a detailed chemo-dynamical view of the disk and bulge of our Galaxy. Our findings on the Milky Way can be linked to the evolution of high redshift disk galaxies, helping to solve the conundrum of galaxy formation.},
  language  = {en}
}
@misc{ThonigDelRioKieferetal.2020,
  author    = {Thonig, Richard and Del Rio, Pablo and Kiefer, Christoph and Lazaro Touza, Lara and Escribano, Gonzalo and Lechon, Yolanda and Spaeth, Leonhard and Wolf, Ingo and Lilliestam, Johan},
  title     = {Does ideology influence the ambition level of climate and renewable energy policy?},
  series = {Zweitver{\"o}ffentlichungen der Universit{\"a}t Potsdam : Wirtschafts- und Sozialwissenschaftliche Reihe},
  journal   = {Zweitver{\"o}ffentlichungen der Universit{\"a}t Potsdam : Wirtschafts- und Sozialwissenschaftliche Reihe},
  number    = {1},
  issn      = {1867-5808},
  doi       = {10.25932/publishup-57798},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-577981},
  pages     = {19},
  year      = {2020},
  abstract  = {We investigate whether political ideology has an observable effect on decarbonization ambition, renewable power aims, and preferences for power system balancing technologies in four European countries. Based on the Energy Logics framework, we identify ideologically different transition strategies (state-centered, market-centered, grassroots-centered) contained in government policies and opposition party programs valid in 2019. We compare these policies and programs with citizen poll data. We find that ideology has a small effect: governments and political parties across the spectrum have similar, and relatively ambitious, decarbonization and renewables targets. This mirrors citizens' strong support for ambitious action regardless of their ideological self-description. However, whereas political positions on phasing out fossil fuel power are clear across the policy space, positions on phasing in new flexibility options to balance intermittent renewables are vague or non-existent. As parties and citizens agree on strong climate and renewable power aims, the policy ambition is likely to remain high, even if governments change.},
  language  = {en}
}