TY - THES A1 - Ganse, Urs T1 - Kinetische Simulationen solarer Typ II Radiobursts T1 - Kinetic Simulations of Solar Type II Radio Bursts N2 - Die Emission solarer Typ II Radiobursts ist ein seit Jahrzehnten beobachtetes Phänomen der heliosphärischen Plasmaphysik. Diese Radiobursts, die im Zusammenhang mit der Propagation koronaler Schockfronten auftreten, zeigen ein charakteristisches, zweibandiges Emissionsspektrum. Mit expandierendem Schock driften sie zu niedrigeren Frequenzen. Analytische Theorien dieser Emission sagen nichtlineare Plasmawellenwechselwirkung als Ursache voraus, doch aufgrund des geringen Sonnenabstands der Emissionsregion ist die in-situ Datenlage durch Satellitenmessungen äusserst schlecht, so dass eine endgültige Verifikation der vorhergesagten Vorgänge bisher nicht möglich war. Mit Hilfe eines kinetischen Plasma-Simulationscodes nach dem Particle-in-Cell Prinzip wurde in dieser Dissertation die Plasmaumgebung in der Foreshock-Region einer koronalen Schockfront modelliert. Das Propagations- und Kopplungsverhalten elektrostatischer und elektromagnetischer Wellenmoden wurde untersucht. Die vollständige räumliche Information über die Wellenzusammensetzung in der Simulation erlaubt es, die Kinematik nichtlinearer Wellenkopplungen genauestens zu untersuchen. Es zeigte sich ein mit der analytischen Theorie der Drei-Wellen-Wechselwirkung konsistentes Bild der Erzeugung solarer Radiobursts: durch elektromagnetischen Zerfall elektrostatischer Moden kommt es zur Erzeugung fundamentaler, sowie durch Verschmelzung gegenpropagierender elektrostatischer Moden zur Anregung harmonischer Radioemission. Kopplungsstärken und Winkelabhängigkeit dieser Prozesse wurden untersucht. Mit dem somit zur Verfügung stehenden, numerischen Laborsystem wurde die Parameter-Abhängigkeit der Wellenkopplungen und entstehenden Radioemissionen bezüglich Stärke des Elektronenbeams und des solaren Abstandes untersucht. N2 - The emission of solar type II radiobursts is a phenomenon of heliospheric plasma physics which has been observed for several decades. These radio bursts, which appear in conjunction with propagating coronal shocks, show a characteristic two-banded emission spectrum, drifting towards lower frequencies as the shock expands. Analytic theories predict nonlinear plasma wave interaction as the cause of these emissions. However, due to its low solar distance, in-situ satellite measurements of the emission regions’ properties are extremely scarce. Hence, a conclusive verification of the predicted processes was hitherto not attainable. Using a kinetic plasma simulation code based on the particle-in-cell approach, the plasma environment in a coronal shock’s foreshock region was modelled in this thesis. The propagation and coupling behaviour of electrostatic and electromagnetic wavemodes was investigated. Complete spatial information of the wave composition as obtainable from the simulations allowed to finely analyze the kinematics of nonlinear wave interactions. The results showed excitation of solar radiobursts in agreement with analytics predictions of three wave interaction processes, based on the nonlinear processes: electromagnetic decay of electrostatic modes is responsible for the fundamental and coalcescense of counterpropagating electrostatic waves responsable for the harmonic radio emission. Coupling strengths and angular dependences of these processes were then studied. With the numerical laboratory system obtained through this modelling effort, the parameter dependence of wave copulings and resulting radio emissions were explored, based on variation of electron beam strength and solar distance of the emission region. KW - Heliosphäre KW - Burst KW - Mathematisches Modell KW - Heliosphere KW - Plasma Physics KW - Electromagnetic Waves KW - Electrostatic Waves KW - Nonlinear Interaction KW - Plasma KW - Elektromagnetische Welle KW - Elektrostatische Welle Y1 - 2012 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:bvb:20-opus-73676 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 -