Moralische Anstalten für die Schaubühne? : zur Poetik von Hochhuths Dramen

Der (...) Beitrag setzt sich strukturell auf drei Ebenen mit Rolf Hochhuths Dramenpoetik auseinander. Erstens wird die gegenläufige Beziehung zwischen ihrem historisch-adäquaten Gestaltungsanspruch und ihrer literarisch-symbolhaften Überformung analysiert. Zweitens wird Hochhuths Verhältnis zu den für ihn poetologisch bedeutsamen Vorgängern Lessing und Schiller untersucht. Drittens geht es um die Frage, welche Konsequenzen sich aus der in den »Guerillas« formulierten Darstellungsabsicht ziehen lassen, der realen Wirklichkeit durch die Projektion einen neuen (literarischen) Wirklichkeit entgegenzutreten

Effects of physical and social environment on zebra finches’ foraging intensity

The zebra finch (Taeniopygia guttata) is the most widely used passerine bird in captive research, yet little work has been done in the wild where physical and social conditions are more variable and their behaviour can be investigated in an ecological context. Zebra finches forage on the ground and are vulnerable to predation by a range of terrestrial and aerial predators. In this thesis, I explore how the physical and social environment affects their foraging decisions in captivity and in the wild. The decision to feed in a particular patch is an attempt to optimise the costs and benefits of feeding at that location. I used giving-up densities (GUD) – the density of food remaining in a patch after the forager(s) have exploited it, to measure the perceived risk of zebra finches to a variety of experimental treatments. In captivity, I investigated how zebra finches’ foraging intensity responded to characteristics of the captive environment such as the availability of perches, cover, and ground substrate. In the wild, I examined how their foraging intensity was affected by the distance to natural cover (vegetation) or their visual fields. I also explored effects of the local neighbourhood density of zebra finches in the wild. I further investigated captive zebra finches’ foraging intensity in different sized groups, as a function of the proximity to, and behaviour of neighbouring flocks. I show that zebra finches forage more intensively when they are close to vegetation and perceive cover as protective. I also found that foraging intensity increased non-linearly with group size and mass and sex mitigated how social and physical environments affected foraging intensity. Overall, my finding suggest that while foraging, zebra finches place greater emphasis on their social, compared to physical environments. My thesis highlights the importance of taking into account a wide range of social factors when investigating foraging decisions by animals

Multi-Wavelength Observations of the High-Mass Star Forming Complexes W33 and DR 21

High-mass stars play a key role in shaping the Universe. Stars with masses above 8 M_sun have a huge impact on the energy budget of galaxies, through their stellar winds, expanding HII regions, outflows, and supernova explosions. Although insight into the formation of stars is gained from low-mass star forming regions, the knowledge about high-mass star formation is still incomplete and has to be increased through new observations and theories. Observationally, different stages of star formation are distinguished. A cold molecular cloud collapses and fragments into smaller entities ("clumps" and "cores"). The cores contract further and slowly start to warm up their center where a protostar is formed. The protostar grows through accretion of material while at a certain point, hydrogen burning sets in. The evolving protostar starts to heat up its birth cloud, changing the chemistry in different layers around the star (hot core phase). An HII region is formed once the radiation of the protostar is energetic enough to ionize the surrounding material. With time, the radiation of the protostar destroys the birth cloud and the star becomes observable at optical wavelengths. In the course of this dissertation, the formation of high-mass stars was studied along the described evolutionary sequence on the basis of multi-wavelength observations of the high-mass star forming complexes W33 and DR 21. In W33, molecular clouds in several stages of star formation are detected, from quiescent cold clouds to highly active HII regions. Two radial velocity components with a difference of ~20 km/s were detected towards different parts of the complex. For a long time, this raised the question if W33 is a physically connected star forming complex or if the star forming regions with different radial velocities are located at different distances along the line-of-sight. Due to this peculiar velocity structure, the distance to W33 was not well known. As part of the dissertation, the trigonometric parallax distance of W33 was determined with Very Long Baseline Interferometry observations of water masers in the complex, yielding a distance of 2.4 kpc. Since the star forming regions with the different radial velocity components are located at similar distances, we conclude that W33 is physically connected. Furthermore, these observations yield the proper motions of the water masers from which we inferred the internal motions of the star forming regions and the motions of these regions within the W33 complex. Since the clouds in the W33 complex are physically linked and are in different stages of star formation, we conducted a chemical study of these clouds with single dish and interferometer observations at submillimeter wavelengths to gather information about the chemical composition on different scales along the evolutionary sequence. On larger scales, the number of detected molecules and their complexity increases from the prestellar phase to the HII region phase. On smaller scales, the clouds in the hot core phase show the highest chemical complexity and diversity. The observed molecules, some of them quite complex, were generated on the dust grains and then released into the gas phase as primary molecules or produced in the gas phase by the evaporated molecules as secondary molecules. In the HII region phase, almost no complex molecules are detected anymore and the spectrum resembles the spectra of the clouds in the protostellar phase before the excitation of a hot core. The complex molecules are either destroyed by photo-dissociation or their emission is not compact enough to be detected by the interferometer. With interferometer observations at radio wavelengths, we looked for hypercompact and ultracompact HII regions in the W33 Main cloud. We detected an ultracompact HII region and inferred the spectral type of the dominating star which ionizes the surrounding material. The ultracompact HII region has an arc-shape similar to cometary HII regions. Furthermore, water masers and a Class I methanol maser are detected in the W33 Main cloud. While the water masers are probably associated with an outflow in W33 Main, the methanol maser is located offset from any dust or molecular line emission and it is not clear what powers it. DR 21 contains two cometary HII regions, whose sizes classify them as ultracompact and compact HII regions. To study the velocity field of the two HII regions, we analyzed archival radio recombination line observations of DR 21. We detected two velocity components in the tails of both HII regions which indicate the presence of stellar winds. Stellar winds clear cavities around the stars and confine the ionized gas in thin shells around these cavities. The two velocity components probably originate from ionized gas at the near and the far side of these shells. The velocity distribution of both HII regions is best explained with a combination of bow shock and champagne flow models. The moving star produces a bow shock at the head of the cometary HII regions, increasing the velocity of the ionized gas compared to the systemic velocity of the neutral material. Increasing velocities of the ionized gas down both tails indicate the presence of a density gradient in the surrounding neutral material (champagne flow model). The density gradient in the southern HII region has been tentatively shown in molecular line observations of DR 21 but has to be confirmed with observations at higher spatial resolution

Patterning of Indium Tin Oxide Films

A relatively rapid, economical process has been devised for patterning a thin film of indium tin oxide (ITO) that has been deposited on a polyester film. ITO is a transparent, electrically conductive substance made from a mixture of indium oxide and tin oxide that is commonly used in touch panels, liquid-crystal and plasma display devices, gas sensors, and solar photovoltaic panels. In a typical application, the ITO film must be patterned to form electrodes, current collectors, and the like. Heretofore it has been common practice to pattern an ITO film by means of either a laser ablation process or a photolithography/etching process. The laser ablation process includes the use of expensive equipment to precisely position and focus a laser. The photolithography/etching process is time-consuming. The present process is a variant of the direct toner process an inexpensive but often highly effective process for patterning conductors for printed circuits. Relative to a conventional photolithography/ etching process, this process is simpler, takes less time, and is less expensive. This process involves equipment that costs less than $500 (at 2005 prices) and enables patterning of an ITO film in a process time of less than about a half hour

Rocket Cratering in Simulated Lunar and Martian Environments

With NASA's planned return to the moon and possibly with lunar outposts being formed, repeated landings at the same site will be necessary. Understanding rocket plume interaction with lunar and Martian surfaces is of paramount importance in order to safely land and protect hardware surrounding the landing site. This work will report on results of three small experiments intended to explore plume impingement onto lunar and Martian surfaces: Handheld Observation of Scour Holes (HOOSH), Handheld Angle of Repose Measurements of Lunar Simulants (HARMLuS), and Mars Architecture Team study (MATS). The first two experiments were performed during two sorties of reduced gravity flights. HOOSH was designed to investigate crater formation as a function of gravitational level (lunar and Martian gravity). HARMLuS was designed to measure the Angle of Failure (related to the angle of repose) at lunar and Martian gravity. Both experiments have complex findings indicative of the hysteretic behavior of granular materials, especially resulting from reduced gravity. The MATS experiment was designed to investigate the effects of regolith compaction on the granular mechanics of crater formation. In general, the granular mechanics is a much stronger function of compaction than gravitation acceleration. Crater formation is greatly enhanced at reduced gravity (resulting in much larger craters). The angle of failure of the lunar simulants increases with decreasing gravitational acceleration, and occasionally becomes infinite for some compactions at lunar gravity. The angle of failure also increases with increasing compaction. While compaction does play a role in the time development of crater formation, the asymptotic behavior is largely unaffected.Comment: 9 pages, 8 figures. Presented at Earth & Space 2010 conferenc

Rocket Cratering in Simulated Lunar and Martian Environments

With NASA's planned return to the moon and possibly with lunar outposts being formed, repeated landings at the same site will be necessary. Understanding rocket plume interaction with lunar and Martian surfaces is of paramount importance in order to safely land and protect hardware surrounding the landing site. This work will report on results of three small experiments intended to explore plume impingement onto lunar and Martian surfaces: Handheld Observation of Scour Holes (HOOSH), Handheld Angle of Repose Measurements of Lunar Simulants (HARMLuS), and Mars Architecture Team study (MATS). The first two experiments were performed during two sorties of reduced gravity flights. HOOSH was designed to investigate crater formation as a function of gravitational level (lunar and Martian gravity). HARMLuS was designed to measure the Angle of Failure (related to the angle of repose) at lunar and Martian gravity. Both experiments have complex findings indicative of the hysteretic behavior of granular materials, especially resulting from reduced gravity. The MATS experiment was designed to investigate the effects of regolith compaction on the granular mechanics of crater formation . In general, the granular mechanics is a much stronger function of compaction than gravitation acceleration. Crater formation is greatly enhanced at reduced gravity (resulting in much larger craters). The angle of failure of the lunar simulants increases with decreasing gravitational acceleration, and occasionally becomes infinite for some compactions at lunar gravity. The angle of failure also increases with increasing compaction. While compaction does play a role in the time development of crater formation, the asymptotic behavior is largely unaffected

Trigonometric Parallaxes of Massive Star Forming Regions: G012.88+0.48 and W33

We report trigonometric parallaxes for water masers in the G012.88+0.48 region and in the massive star forming complex W33 (containing G012.68--0.18, G012.81--0.19, G012.90--0.24, G012.90--0.26), from the Bar and Spiral Structure Legacy (BeSSeL) survey using the Very Long Baseline Array. The parallax distances to all these masers are consistent with $2.40^{+0.17}_{-0.15}$ kpc, which locates the W33 complex and G012.88+0.48 in the Scutum spiral arm. Our results show that W33 is a single star forming complex at about two-thirds the kinematic distance of 3.7 kpc. The luminosity and mass of this region, based on the kinematic distance, have therefore been overestimated by more than a factor of two. The spectral types in the star cluster in W33\,Main have to be changed by 1.5 points to later types.Comment: 9 pages, 11 figures, 2 tables; accepted for publication at A&