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David Orozco Suárez (Instituto de Astrofísica de Andalucía)23/06/2016, 09:00Spectropolarimetry in the He I 1083nm multiplet offers a unique opportunity to observe magnetic fields in the chromosphere. There, the magnetic fields are expected to be much lower in intensity than in the photosphere. In this regard, the polarization signals of the He I 1083nm multiplet are sensitive to atomic level polarization and to the joint action of the Hanle and...Go to contribution page
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Peter Levens (University of Glasgow)23/06/2016, 09:30Coordinated observations of solar prominences can be a challenge to perform, and even more so to analyse. During international campaigns in 2014 and 2015 we focused on studying tornado-like prominences with a combination of space-based satellites (IRIS, Hinode and SDO) and ground based telescopes (THEMIS, Meudon MSDP). We measured the magnetic field strength and orientation in these...Go to contribution page
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Lakshmi Pradeep Chitta (Max Planck Institute for Solar System Research)23/06/2016, 09:50Magnetic reconnection is thought to be responsible for eruptive events on the Sun, from large-scale CMEs to small-scale events that are barely resolved. The height in the solar atmosphere where the reconnection takes place may significantly influence the morphology and appearance of the events. This might be the main distinction between events such as e.g. Ellerman bombs, IRIS bombs, or...Go to contribution page
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Maria Loukitcheva (Max-Planck-Institut fuer Sonnensystemforschung)23/06/2016, 10:10Atacama Large Millimeter/Submillimeter Array (ALMA) is opening a new chapter in the study of the Sun by providing a leap in spatial resolution and sensitivity compared to currently available millimeter wavelength observations. Using state of the art radiation MHD simulations of the solar atmosphere we demonstrate the huge potential of ALMA observations for uncovering the nature of the...Go to contribution page
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Patrick Antolin (School of Mathematics and Statistics, University of St Andrews)23/06/2016, 11:15The solar atmosphere is permeated with MHD waves of Alfvenic character. Such waves are considered important energy carriers through which the heating and morphology of the corona may be explained. The highly inhomogeneous coronal environment, particularly in solar prominences, ensures the co-existence of different wave modes that are expected to be coupled through the robust...Go to contribution page
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Manuel Luna (Instituto de Astrofísica de Canarias (IAC))23/06/2016, 11:45Large-amplitude oscillations in prominences are among the most spectacular phenomena of the solar atmosphere. Such an oscillations involve motions with velocities above 20 km/s, and large portions of the filament that move in phase. These are triggered by energetic disturbances as flares and jets. These oscillations are an excellent tool to probe the not directly measurable filament...Go to contribution page
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Huadong Chen (National Astronomical Observatories, Chinese Academy of Sciences)23/06/2016, 12:05Triggering mechanisms of solar eruptions have long been a challenge. A few previous case studies have indicated that preceding gentle filament merging via magnetic reconnection may launch following intense eruption, according to the tether-cutting (TC) model. However, the detailed process of TC reconnection between filaments has not been exhibited yet. In this work, we report the...Go to contribution page
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Takafumi Kaneko (The University of Tokyo)23/06/2016, 12:25We show that topological change of coronal magnetic field can trigger radiative condensation for in-situ prominence formation by 3D MHD simulation including thermal conduction and optically thin radiative cooling. The multi-wavelength observation by SDO/AIA (Bergeret al., 2012) has found the process of in-situ prominence formation, in which the cool dense plasma of prominence came from...Go to contribution page
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