Beitrag zur Kenntnis der Copepoda Harpacticoidea sublitoraler Weichböden in der Kieler Bucht

Von September 1968 bis August 1969 wurde die Harpacticidenfauna der sublitoralen Weichböden in der östlichen Kieler Bucht untersucht. Von den 31 aufgefundenen Arten erwiesen sich 11 als neu für das Gebiet der Kieler Bucht. Eine neue Unterart konnte beschrieben werden: Robertsonia tenuis (BRADY u. ROBERTSON) kieliensis ssp. nov. Bei folgenden Arten werden taxonomische Fragen erörtert: Halectinosoma herdmani, Haleclinosoma fumarchium, Pseudobradya minor, Robertsonia tenuis, Typhlamphiascus typhlops, Amphiascoides debilis, Amphiascoides dispar und Arthropsyllus serratus. Ferner werden einige ökologische Gesichtspunkte behandelt. The Copepoda Harpacticoidea of sublitoral muddy bottoms in the eastern part of the Kieler Bucht were studied from September 1968 till August 1969. From 31 species found 11 are new for the Kieler Bucht region. One new subspecies is described: Roberseniar tenuis (BRADY + ROBERTSON) kieliensis ssp. nov. Besides taxonomical studies concerning the following species, Halectinosoma herdmani, Halectinosoma finmarchicum, Pseudobradya minor, Robertsonia tenuis kieliensis, Typhlamphiascus typhlops, Amphiascoides debilis, Amphiascoides dispar and Arthropsyllus sceratus some ecological aspects are discussed

Logistik der Schüttgüter

Im Auftrag des Präsidenten der Fraunhofer-Gesellschaft hat das Fraunhofer-Institut für Transporttechnik und Warendistribution (ITW) in Dortmund eine umfassend angelegte Studie im Gesamtfeld der Schüttguttechnologie durchgeführt. Von Teilen dieser eigentlich Fraunhofer-internen Studie soll im Rahmen dieses Artikels berichtet werden

Measurement of the cosmic ray spectrum above 4×10184{\times}10^{18} eV using inclined events detected with the Pierre Auger Observatory

A measurement of the cosmic-ray spectrum for energies exceeding $4{\times}10^{18}$ eV is presented, which is based on the analysis of showers with zenith angles greater than $60^{\circ}$ detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above $5.3{\times}10^{18}$ eV, the "ankle", the flux can be described by a power law $E^{-\gamma}$ with index $\gamma=2.70 \pm 0.02 \,\text{(stat)} \pm 0.1\,\text{(sys)}$ followed by a smooth suppression region. For the energy ($E_\text{s}$) at which the spectral flux has fallen to one-half of its extrapolated value in the absence of suppression, we find $E_\text{s}=(5.12\pm0.25\,\text{(stat)}^{+1.0}_{-1.2}\,\text{(sys)}){\times}10^{19}$ eV.Comment: Replaced with published version. Added journal reference and DO

Energy Estimation of Cosmic Rays with the Engineering Radio Array of the Pierre Auger Observatory

The Auger Engineering Radio Array (AERA) is part of the Pierre Auger Observatory and is used to detect the radio emission of cosmic-ray air showers. These observations are compared to the data of the surface detector stations of the Observatory, which provide well-calibrated information on the cosmic-ray energies and arrival directions. The response of the radio stations in the 30 to 80 MHz regime has been thoroughly calibrated to enable the reconstruction of the incoming electric field. For the latter, the energy deposit per area is determined from the radio pulses at each observer position and is interpolated using a two-dimensional function that takes into account signal asymmetries due to interference between the geomagnetic and charge-excess emission components. The spatial integral over the signal distribution gives a direct measurement of the energy transferred from the primary cosmic ray into radio emission in the AERA frequency range. We measure 15.8 MeV of radiation energy for a 1 EeV air shower arriving perpendicularly to the geomagnetic field. This radiation energy -- corrected for geometrical effects -- is used as a cosmic-ray energy estimator. Performing an absolute energy calibration against the surface-detector information, we observe that this radio-energy estimator scales quadratically with the cosmic-ray energy as expected for coherent emission. We find an energy resolution of the radio reconstruction of 22% for the data set and 17% for a high-quality subset containing only events with at least five radio stations with signal.Comment: Replaced with published version. Added journal reference and DO

Measurement of the Radiation Energy in the Radio Signal of Extensive Air Showers as a Universal Estimator of Cosmic-Ray Energy

We measure the energy emitted by extensive air showers in the form of radio emission in the frequency range from 30 to 80 MHz. Exploiting the accurate energy scale of the Pierre Auger Observatory, we obtain a radiation energy of 15.8 \pm 0.7 (stat) \pm 6.7 (sys) MeV for cosmic rays with an energy of 1 EeV arriving perpendicularly to a geomagnetic field of 0.24 G, scaling quadratically with the cosmic-ray energy. A comparison with predictions from state-of-the-art first-principle calculations shows agreement with our measurement. The radiation energy provides direct access to the calorimetric energy in the electromagnetic cascade of extensive air showers. Comparison with our result thus allows the direct calibration of any cosmic-ray radio detector against the well-established energy scale of the Pierre Auger Observatory.Comment: Replaced with published version. Added journal reference and DOI. Supplemental material in the ancillary file

Active Galactic Nuclei: Sources for ultra high energy cosmic rays?

The origin of ultra high energy cosmic rays promises to lead us to a deeper understanding of the structure of matter. This is possible through the study of particle collisions at center-of-mass energies in interactions far larger than anything possible with the Large Hadron Collider, albeit at the substantial cost of no control over the sources and interaction sites. For the extreme energies we have to identify and understand the sources first, before trying to use them as physics laboratories. Here we describe the current stage of this exploration. The most promising contenders as sources are radio galaxies and gamma ray bursts. The sky distribution of observed events yields a hint favoring radio galaxies. Key in this quest are the intergalactic and galactic magnetic fields, whose strength and structure are not yet fully understood. Current data and statistics do not yet allow a final judgment. We outline how we may progress in the near future.Comment: proceedings for "Origin, Mass, Composition and Acceleration Mechanisms of UHECRs (CRIS 2008)" in Malfa (Salina Island - Italy) on September 15-19, 200