TY - JOUR A1 - Kilian, Yvonne A1 - Wehmeier, Udo F. A1 - Wahl, Patrick A1 - Mester, Joachim A1 - Hilberg, Thomas A1 - Sperlich, Billy T1 - Acute Response of Circulating Vascular Regulating MicroRNAs during and after High-Intensity and High-Volume Cycling in Children JF - Frontiers in Physiology N2 - Aim: The aim of the present study was to analyze the response of vascular circulating microRNAs (miRNAs; miR-16, miR-21, miR-126) and the VEGF mRNA following an acute bout of HIIT and HVT in children. Methods: Twelve healthy competitive young male cyclists (14.4 ± 0.8 years; 57.9 ± 9.4 ml•min−1•kg−1 peak oxygen uptake) performed one session of high intensity 4 × 4 min intervals (HIIT) at 90–95% peak power output (PPO), each interval separated by 3 min of active recovery, and one high volume session (HVT) consisting of a constant load exercise for 90 min at 60% PPO. Capillary blood from the earlobe was collected under resting conditions, during exercise (d1 = 20 min, d2 = 30 min, d3 = 60 min), and 0, 30, 60, 180 min after the exercise to determine miR-16, -21, -126, and VEGF mRNA. Results: HVT significantly increased miR-16 and miR-126 during and after the exercise compared to pre-values, whereas HIIT showed no significant influence on the miRNAs compared to pre-values. VEGF mRNA significantly increased during and after HIIT (d1, 30′, 60′, 180′) and HVT (d3, 0′, 60′). Conclusion: Results of the present investigation suggest a volume dependent exercise regulation of vascular regulating miRNAs (miR-16, miR-21, miR-126) in children. In line with previous data, our data show that acute exercise can alter circulating miRNAs profiles that might be used as novel biomarkers to monitor acute and chronic changes due to exercise in various tissues. KW - children KW - endurance KW - exercise KW - microRNAs KW - training adaptation Y1 - 2016 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:bvb:20-opus-165261 VL - 7 IS - 92 ER - TY - JOUR A1 - Vainio, Rami A1 - Valtonen, Eino A1 - Heber, Bernd A1 - Malandraki, Olga E. A1 - Papaioannou, Athanasios A1 - Klein, Karl-Ludwig A1 - Afanasiev, Alexander A1 - Agueda, Neus A1 - Aurass, Henry A1 - Battarbee, Markus A1 - Braune, Stephan A1 - Dröge, Wolfgang A1 - Ganse, Urs A1 - Hamadache, Clarisse A1 - Heynderickx, Daniel A1 - Huttunen-Heikinmaa, Kalle A1 - Kiener, Jürgen A1 - Kilian, Patrick A1 - Kopp, Andreas A1 - Kouloumvakos, Athanasios A1 - Maisala, Sami A1 - Mishev, Alexander A1 - Miteva, Rosita A1 - Nindos, Alexander A1 - Oittinen, Tero A1 - Raukunen, Osku A1 - Riihonen, Esa A1 - Rodriguez-Gasen, Rosa A1 - Saloniemi, Oskari A1 - Sanahuja, Blai A1 - Scherer, Renate A1 - Spanier, Felix A1 - Tatischeff, Vincent A1 - Tziotziou, Kostas A1 - Usoskin, Ilya G. A1 - Vilmer, Nicole T1 - The first SEPServer event catalogue similar to ~68-MeV solar proton events observed at 1 AU in 1996-2010 JF - Journal of Space Weather and Space Climate N2 - SEPServer is a three-year collaborative project funded by the seventh framework programme (FP7-SPACE) of the European Union. The objective of the project is to provide access to state-of-the-art observations and analysis tools for the scientific community on solar energetic particle (SEP) events and related electromagnetic (EM) emissions. The project will eventually lead to better understanding of the particle acceleration and transport processes at the Sun and in the inner heliosphere. These processes lead to SEP events that form one of the key elements of space weather. In this paper we present the first results from the systematic analysis work performed on the following datasets: SOHO/ERNE, SOHO/EPHIN, ACE/EPAM, Wind/WAVES and GOES X-rays. A catalogue of SEP events at 1 AU, with complete coverage over solar cycle 23, based on high-energy (similar to 68-MeV) protons from SOHO/ERNE and electron recordings of the events by SOHO/EPHIN and ACE/EPAM are presented. A total of 115 energetic particle events have been identified and analysed using velocity dispersion analysis (VDA) for protons and time-shifting analysis (TSA) for electrons and protons in order to infer the SEP release times at the Sun. EM observations during the times of the SEP event onset have been gathered and compared to the release time estimates of particles. Data from those events that occurred during the European day-time, i.e., those that also have observations from ground-based observatories included in SEPServer, are listed and a preliminary analysis of their associations is presented. We find that VDA results for protons can be a useful tool for the analysis of proton release times, but if the derived proton path length is out of a range of 1 AU < s less than or similar to 3 AU, the result of the analysis may be compromised, as indicated by the anti-correlation of the derived path length and release time delay from the associated X-ray flare. The average path length derived from VDA is about 1.9 times the nominal length of the spiral magnetic field line. This implies that the path length of first-arriving MeV to deka-MeV protons is affected by interplanetary scattering. TSA of near-relativistic electrons results in a release time that shows significant scatter with respect to the EM emissions but with a trend of being delayed more with increasing distance between the flare and the nominal footpoint of the Earth-connected field line. KW - radio emissions (dynamic) KW - projects KW - advanced composition explorer KW - wind spacecraft KW - stereo mission KW - alpha monitor KW - electron KW - plasma KW - radio KW - spectrometer KW - heliosphere KW - instrument KW - radiation KW - flares Y1 - 2013 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:bvb:20-opus-122847 SN - 2115-7251 VL - 3 IS - A12 ER - TY - THES A1 - Kilian, Patrick T1 - Teilchenbeschleunigung an kollisionsfreien Schockfronten T1 - Partical acceleration at collisionless shock fronts N2 - Das Magnetfeld der Sonne ist kein einfaches statisches Dipolfeld, sondern weist wesentlich kompliziertere Strukturen auf. Wenn Rekonnexion die Topologie eines Feldlinienbündels verändert, wird viel Energie frei, die zuvor im Magnetfeld gespeichert war. Das abgetrennte Bündel wird mit dem damit verbundenen Plasma mit großer Geschwindigkeit durch die Korona von der Sonne weg bewegen. Dieser Vorgang wird als koronaler Massenauswurf bezeichnet. Da diese Bewegung mit Geschwindigkeiten deutlich über der Alfv\'en-Geschwindigkeit, der kritischen Geschwindigkeit im Sonnenwind, erfolgen kann, bildet sich eine Schockfront, die durch den Sonnenwind propagiert. Satelliten, die die Bedingungen im Sonnenwind beobachten, detektieren beim Auftreten solcher Schockfronten einen erhöhten Fluss von hochenergetischen Teilchen. Mit Radioinstrumenten empfängt man zeitgleich elektromagnetische Phänomene, die als Radiobursts bezeichnet werden, und ebenfalls für die Anwesenheit energiereicher Teilchen sprechen. Daher, und aufgrund von theoretischen Überlegungen liegt es nahe, anzunehmen, daß Teilchen an der Schockfront beschleunigt werden können. Die Untersuchung der Teilchenbeschleunigung an kollisionsfreien Schockfronten ist aber noch aus einem zweiten Grund interessant. Die Erde wird kontinuierlich von hochenergetischen Teilchen, die aus historischen Gründen als kosmische Strahlung bezeichnet werden, erreicht. Die gängige Theorie für deren Herkunft besagt, daß zumindest der galaktische Anteil durch die Beschleunigung an Schockfronten, die durch Supernovae ausgelöst wurden, bis zu den beobachteten hohen Energien gelangt sind. Das Problem bei der Untersuchung der Herkunft der kosmischen Strahlung ist jedoch, daß die Schockfronten um Supernovaüberreste aufgrund der großen Entfernung nicht direkt beobachtbar sind. Es liegt dementsprechend nahe, die Schockbeschleunigung an den wesentlich näheren und besser zu beobachtenden Schocks im Sonnensystem zu studieren, um so Modelle und Simulationen entwickeln und testen zu können. Die vorliegende Arbeit beschäftigt sich daher mit Simulationen von Schockfronten mit Parametern, die etwa denen von CME getriebenen Schocks entsprechen. Um die Entwicklung der Energieverteilung der Teilchen zu studieren, ist ein kinetischer Ansatz nötig. Dementsprechend wurden die Simulationen mit einem Particle-in-Cell Code durchgeführt. Die Herausforderung ist dabei die große Spanne zwischen den mikrophysikalischen Zeit- und Längenskalen, die aus Gründen der Genauigkeit und numerischen Stabilität aufgelöst werden müssen und den wesentlich größeren Skalen, die die Schockfront umfasst und auf der Teilchenbeschleunigung stattfindet. Um die Stabilität und physikalische Aussagekraft der Simulationen sicherzustellen, werden die numerischen Bausteine mittels Testfällen, deren Verhalten bekannt ist, gründlich auf ihre Tauglichkeit und korrekte Implementierung geprüft. Bei den resultierenden Simulationen wird das Zutreffen von analytischen Vorhersagen (etwa die Einhaltung der Sprungbedingungen) überprüft. Auch die Vorhersagen einfacherer Plasmamodelle, etwa für das elektrostatischen Potential an der Schockfront, das man auch aus einer Zwei-Fluid-Beschreibung erhalten kann, folgen automatisch aus der selbstkonsistenten, kinetischen Beschreibung. Zusätzlich erhält man Aussagen über das Spektrum und die Bahnen der beschleunigten Teilchen. N2 - The magnetic field of the sun is not a simple static dipole field but comprises much more complicated structures. When magnetic reconnection changes the topology of a structure the large amount of energy that was stored in the magnetic field is released and can eject the remainder of the magnetic structure and the plasma that is frozen to the magnetic field lines from the solar corona at large velocities. This event is called a coronal mass ejection (CME). Given that the upward motion happens at velocities larger than the local Alfv\'en speed, the critical speed in the solar wind, the CME will act as a piston that drives a shock front through the solar wind ahead of itself. Satellites that monitor solar wind conditions detect an enhanced flux of high energy particles associated with the shock front. Radio instruments typically pick up bursts of electromagnetic emission, termed radio bursts, that are also consistent with processes driven by energetic particles. Thus, and due to theoretical considerations, it is safe to assume that particles can be accelerated at the shock front. Particle acceleration at collisionless shock fronts is an interesting topic for another reason. Earth is constantly bombarded by very energetic particles called (due to historical reasons) cosmic rays. The leading theory for the production of at least the fraction of cosmic rays that originate in our galaxy is acceleration at shock fronts, e.g. in super nova remnants. The large distance and consequently limited observation of these shock fronts restrict more detailed investigations. It is therefore useful to study the process of shock acceleration at shocks in the solar system that are much closer and more approachable to develop and test models and simulation methods that can be applied in different regimes. This dissertation aims at simulations of shock fronts with parameters that are close to the ones occurring in CME driven shocks. Since the goal is the investigation of the changing particle spectrum fully kinetic methods are necessary and consequently a particle in cell code was developed and used. The main challenge there is the large span of time and length scales that range from the microscopic regime that has to be resolved to guarantee stability and accuracy to the much larger scales of the entire shock fronts at which the particle acceleration takes place. To prove the numerical stability and suitability of the simulations to provide physical results all numerical building blocks are tested on problems where the correct behavior is known to verify the correct implementation. For validation purposes the results of the final shock simulations are compared with analytic predictions (such as the jump conditions from magneto hydrodynamics) and predictions of simpler plasma models (such as the cross shock potential that can be derived from two fluid theory). Finally results that can only be obtained from a self consistent, fully kinetic model, such as particle spectra and trajectories, are discussed. KW - Stoßfreies Plasma KW - Sonnenwind KW - Teilchenbeschleunigung KW - Computersimulation KW - kinetische Plasmaphysik KW - Stoßwelle KW - Schockfront Y1 - 2015 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:bvb:20-opus-119023 ER - TY - JOUR A1 - Vogel, Patrick A1 - Markert, Jonathan A1 - Rückert, Martin A. A1 - Herz, Stefan A1 - Keßler, Benedikt A1 - Dremel, Kilian A1 - Althoff, Daniel A1 - Weber, Matthias A1 - Buzug, Thorsten M. A1 - Bley, Thorsten A. A1 - Kullmann, Walter H. A1 - Hanke, Randolf A1 - Zabler, Simon A1 - Behr, Volker C. T1 - Magnetic Particle Imaging meets computed tomography: first simultaneous imaging JF - Scientific Reports N2 - Magnetic Particle Imaging (MPI) is a promising new tomographic modality for fast as well as three-dimensional visualization of magnetic material. For anatomical or structural information an additional imaging modality such as computed tomography (CT) is required. In this paper, the first hybrid MPI-CT scanner for multimodal imaging providing simultaneous data acquisition is presented. KW - Applied physics KW - Biomedical engineering KW - Imaging techniques Y1 - 2019 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:bvb:20-opus-202501 VL - 9 ER -