Stabilität und Transport in der planetaren Grenzschicht - Untersuchungen mit Radiosonden- und Spurengasmessungen während PARADE

Die vorliegende Arbeit untersucht die Struktur und Zusammensetzung der untersten Atmosphäre im Rahmen der PARADE-Messkampagne (PArticles and RAdicals: Diel observations of the impact of urban and biogenic Emissions) am Kleinen Feldberg in Deutschland im Spätsommer 2011. Dazu werden Messungen von meteorologischen Grundgrößen (Temperatur, Feuchte, Druck, Windgeschwindigkeit und -richtung) zusammen mit Radiosonden und flugzeuggetragenen Messungen von Spurengasen (Kohlenstoffmonoxid, -dioxid, Ozon und Partikelanzahlkonzentrationen) ausgewertet. Ziel ist es, mit diesen Daten, die thermodynamischen und dynamischen Eigenschaften und deren Einfluss auf die chemische Luftmassenzusammensetzung in der planetaren Grenzschicht zu bestimmen. Dazu werden die Radiosonden und Flugzeugmessungen mit Lagrangeschen Methoden kombiniert und es wird zwischen rein kinematischen Modellen (LAGRANTO und FLEXTRA) sowie sogenannten Partikeldispersionsmodellen (FLEXPART) unterschieden. Zum ersten Mal wurde im Rahmen dieser Arbeit dabei auch eine Version von FLEXPART-COSMO verwendet, die von den meteorologischen Analysefeldern des Deutschen Wetterdienstes angetrieben werden. Aus verschiedenen bekannten Methoden der Grenzschichthöhenbestimmung mit Radiosondenmessungen wird die Bulk-Richardson-Zahl-Methode als Referenzmethode verwendet, da sie eine etablierte Methode sowohl für Messungen und als auch Modellanalysen darstellt. Mit einer Toleranz von 125 m, kann zu 95 % mit mindestens drei anderen Methoden eine Übereinstimmung zu der ermittelten Grenzschichthöhe festgestellt werden, was die Qualität der Grenzschichthöhe bestätigt. Die Grenzschichthöhe variiert während der Messkampagne zwischen 0 und 2000 m über Grund, wobei eine hohe Grenzschicht nach dem Durchzug von Kaltfronten beobachtet wird, hingegen eine niedrige Grenzschicht unter Hochdruckeinfluss und damit verbundener Subsidenz bei windarmen Bedingungen im Warmsektor. Ein Vergleich zwischen den Grenzschichthöhen aus Radiosonden und aus Modellen (COSMO-DE, COSMO-EU, COSMO-7) zeigt nur geringe Unterschiede um -6 bis +12% während der Kampagne am Kleinen Feldberg. Es kann allerdings gezeigt werden, dass in größeren Simulationsgebieten systematische Unterschiede zwischen den Modellen (COSMO-7 und COSMO-EU) auftreten. Im Rahmen dieser Arbeit wird deutlich, dass die Bodenfeuchte, die in diesen beiden Modellen unterschiedlich initialisiert wird, zu verschiedenen Grenzschichthöhen führt. Die Folge sind systematische Unterschiede in der Luftmassenherkunft und insbesondere der Emissionssensitivität. Des Weiteren kann lokale Mischung zwischen der Grenzschicht und der freien Troposphäre bestimmt werden. Dies zeigt sich in der zeitlichen Änderung der Korrelationen zwischen CO2 und O3 aus den Flugzeugmessungen, und wird im Vergleich mit Rückwärtstrajektorien und Radiosondenprofilen bestärkt. Das Einmischen der Luftmassen in die Grenzschicht beeinflusst dabei die chemische Zusammensetzung in der Vertikalen und wahrscheinlich auch am Boden. Diese experimentelle Studie bestätigt die Relevanz der Einmischungsprozesse aus der freien Troposphäre und die Verwendbarkeit der Korrelationsmethode, um Austausch- und Einmischungsprozesse an dieser Grenzfläche zu bestimmen.

Analysis of evening and morning transitions in complex terrain: MATERHORN campaign 2013

A field study of thermal circulation over very gentle slope is described for a specific day characterised by weak synoptic conditions. The emphasis was on morning and evening transitions, but measurements cover the entire day; therefore a brief analysis is performed to represent the general thermal circulation pattern. Both transition periods are characterised by complex dynamic behaviours. During evening transition, the upslope flow has got through a stagnation condition characterised by wind velocity U<0:5 m=s. Only when the stagnating air has become negative buoyant, the flow is allowed to pour downslope like a slab. Some features of front formation has been found during the transition development, such as delay time of downslope flow start up along the slope, and the presence of positive turbulent kinetic energy at the onset of the motion. Eventually the observed evening transition has followed a mixed mechanisms, with features from different models. Therefore the Rayleigh number seems not to be a good criterion by which parametrise evening transition itself. Morning transition is characterised by destruction of nocturnal temperature inversion and the onset of upslope flow. Inversion destruction can be described in terms of CBL growth at surface and inversion decent from the top of the layer. KH has found to be a good indicator of inversion breakup, if used as parameter to study the inversion breakup in terms of temperature reversal. After the inversion breakup, buoyancy and mechanical productions supply the flow with the necessary energy to start the upslope wind. More quantitative analysis are provided by the study of stability parameters and turbulent kinetic energy budgets. Gradient Richardson number has been used in this terms, finding that a mixed SBL-CBL behaviour dominates the most of the observed layers. Tke budget has shown high turbulent behaviour during morning transition while the evening transition has developed entirely in laminar condition, apart from short intermittent turbulent events.

THE EFFECTS OF IRRADIATION ON HOT JOVIAN ATMOSPHERES: HEAT REDISTRIBUTION AND ENERGY DISSIPATION

Hot Jupiters, due to the proximity to their parent stars, are subjected to a strong irradiating flux that governs their radiative and dynamical properties. We compute a suite of three-dimensional circulation models with dual-band radiative transfer, exploring a relevant range of irradiation temperatures, both with and without temperature inversions. We find that, for irradiation temperatures T irr lsim 2000 K, heat redistribution is very efficient, producing comparable dayside and nightside fluxes. For T irr ≈ 2200-2400 K, the redistribution starts to break down, resulting in a high day-night flux contrast. Our simulations indicate that the efficiency of redistribution is primarily governed by the ratio of advective to radiative timescales. Models with temperature inversions display a higher day-night contrast due to the deposition of starlight at higher altitudes, but we find this opacity-driven effect to be secondary compared to the effects of irradiation. The hotspot offset from the substellar point is large when insolation is weak and redistribution is efficient, and decreases as redistribution breaks down. The atmospheric flow can be potentially subjected to the Kelvin-Helmholtz instability (as indicated by the Richardson number) only in the uppermost layers, with a depth that penetrates down to pressures of a few millibars at most. Shocks penetrate deeper, down to several bars in the hottest model. Ohmic dissipation generally occurs down to deeper levels than shock dissipation (to tens of bars), but the penetration depth varies with the atmospheric opacity. The total dissipated Ohmic power increases steeply with the strength of the irradiating flux and the dissipation depth recedes into the atmosphere, favoring radius inflation in the most irradiated objects. A survey of the existing data, as well as the inferences made from them, reveals that our results are broadly consistent with the observational trends.

Turbulent flux and meteorological measurements during ARCTEX-2006 campaign

This dataset present result from the DFG- funded Arctic-Turbulence-Experiment (ARCTEX-2006) performed by the University of Bayreuth on the island of Svalbard, Norway, during the winter/spring transition 2006. From May 5 to May 19, 2006 turbulent flux and meteorological measurements were performed on the monitoring field near Ny-Ålesund, at 78°55'24'' N, 11°55'15'' E Kongsfjord, Svalbard (Spitsbergen), Norway. The ARCTEX-2006 campaign site was located about 200 m southeast of the settlement on flat snow covered tundra, 11 m to 14 m above sea level. The permanent sites used for this study consisted of the 10 m meteorological tower of the Alfred Wegener Institute for Polar- and Marine Research (AWI), the international standardized radiation measurement site of the Baseline Surface Radiation Network (BSRN), the radiosonde launch site and the AWI tethered balloon launch sites. The temporary sites - set up by the University of Bayreuth - were a 6 m meteorological gradient tower, an eddy-flux measurement complex (EF), and a laser-scintillometer section (SLS). A quality assessment and data correction was applied to detect and eliminate specific measurement errors common at a high arctic landscape. In addition, the quality checked sensible heat flux measurements are compared with bulk aerodynamic formulas that are widely used in atmosphere-ocean/land-ice models for polar regions as described in Ebert and Curry (1993, doi:10.1029/93JC00656) and Launiainen and Cheng (1995). These parameterization approaches easily allow estimation of the turbulent surface fluxes from routine meteorological measurements. The data show: - the role of the intermittency of the turbulent atmospheric fluctuation of momentum and scalars, - the existence of a disturbed vertical temperature profile (sharp inversion layer) close to the surface, - the relevance of possible free convection events for the snow or ice melt in the Arctic spring at Svalbard, and - the relevance of meso-scale atmospheric circulation pattern and air-mass advection for the near-surface turbulent heat exchange in the Arctic spring at Svalbard. Recommendations and improvements regarding the interpretation of eddy-flux and laser-scintillometer data as well as the arrangement of the instrumentation under polar distinct exchange conditions and (extreme) weather situations could be derived.

(Table 1) Conditions of vertical near-bottom profiling and the main parameters of the benthic boundary layer in several regions of the Black Sea shelf

Measurements of 14 vertical profiles of currents and hydrological parameters in the near-bottom layer with depth resolution of 0.1 m were carried out in several regions of the Black Sea shelf, at five points over the continental slope, and in three deep water regions. The upper boundary of the benthic boundary layer (BBL) was reliably determined at a point at distance from 5-7 to 35-40 m from the bottom where the gradients of density and current velocity changed. Experimental data obtained were used to determine the coefficient of bottom friction, friction velocity, coefficients of vertical diffusion of momentum and density, and vertical fluxes of temperature and salinity in the BBL.

Increasing the genetic uniformity of bighead carp [Aristichthys nobilis (Richardson)] by means of spontaneous diploidization of gynogenetically activated eggs

Three groups of gynogenetic diploid bighead carp were successfully obtained by means of artificial gynogenesis. The activation rates of gynogenesis varied from 75.9% to 98.8%, and the frequency of spontaneous diploidization was around 0.4%. Over 2000 normally gynogenetic diploid fry were obtained in three gynogenetic groups. The haploid karyotype consisted of nine metacentric, 12 submetacentric, three subtelocentric chromosomes and 45 arms. The chromosome number was 48 from gynogenetic diploid. The results showed that the genetic material of offspring was maternal. The aneuploid hybrid embryos of bighead carp and Xingguo red common carp with chromosome numbers ranging from 28 to 73 did not survive post hatch, likely the result of incompatibility between the nucleus and the cytoplasm of two parents. Sixty RAPD primers from three groups were used for total DNA amplification of gynogenetic offspring, maternal and 'paternal' fish. A total of 451 bands were amplified from three kinds of samples above. From maternal bighead carp, 256 bands were amplified; however, there were 251 shared bands between maternal and gynogenetic bighead carp. From artificial gynogenetic offspring, two 'paternal' DNA segments without an expression function were found. An UPGMA tree showed that gynogenetic offspring were closely clustered and the genetic identity among them was very high (0.956).

Scaled Heavy-Ball Acceleration of the Richardson-Lucy Algorithm

The Richardson-Lucy algorithm is one of the most important algorithms in the image deconvolution area. However, one of its drawbacks is slow convergence. A very significant acceleration is obtained by the technique proposed by Biggs and Andrews (BA), which is implemented in the deconvlucy function of the Image Processing MATLAB toolbox. The BA method was developed heuristically with no proof of convergence. In this paper, we introduce the Heavy-Ball (H-B) method for Poisson data optimization and extend it to a scaled H-B method, which includes the BA method as a special case. The method has proof of the convergence rate of O(k-2), where k is the number of iterations. We demonstrate the superior convergence performance of the scaled H-B method on both synthetic and real 3D images.

Scaled Heavy-Ball Acceleration of the Richardson-Lucy Algorithm for 3D Microscopy Image Restoration

The Richardson–Lucy algorithm is one of the most important in image deconvolution. However, a drawback is its slow convergence. A significant acceleration was obtained using the technique proposed by Biggs and Andrews (BA), which is implemented in the deconvlucy function of the image processing MATLAB toolbox. The BA method was developed heuristically with no proof of convergence. In this paper, we introduce the heavy-ball (H-B) method for Poisson data optimization and extend it to a scaled H-B method, which includes the BA method as a special case. The method has a proof of the convergence rateof O(K^2), where k is the number of iterations. We demonstrate the superior convergence performance, by a speedup factor off ive, of the scaled H-B method on both synthetic and real 3D images.

Deviation from quark number scaling of the anisotropy parameter v(2) of pions, kaons, and protons in Au+Au collisions at root s(NN)=200 GeV

Measurements of the anisotropy parameter v(2) of identified hadrons (pions, kaons, and protons) as a function of centrality, transverse momentum p(T), and transverse kinetic energy KET at midrapidity (vertical bar eta vertical bar < 0.35) in Au + Au collisions at root s(N N) = 200 GeV are presented. Pions and protons are identified up to p(T) = 6 GeV/c, and kaons up to p(T) = 4 GeV/c, by combining information from time-of-flight and aerogel Cerenkov detectors in the PHENIX Experiment. The scaling of v(2) with the number of valence quarks (n(q)) has been studied in different centrality bins as a function of transverse momentum and transverse kinetic energy. A deviation from previously observed quark-number scaling is observed at large values of KET/n(q) in noncentral Au + Au collisions (20-60%), but this scaling remains valid in central collisions (0-10%).