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Lucia Kleint (FHNW Switzerland)21/06/2016, 09:00A large part of the energy of solar flares goes into heating, radiation, and mass motion in the lower solar atmosphere. By combining IRIS data with different instruments, such as RHESSI, SDO, and ground-based telescopes, we can infer the properties from the photosphere to the corona during flares. In this talk, I will give an introduction to flare observations with IRIS. IRIS data can...Go to contribution page
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Magnus Woods (UCL-Mullard Space Science Laboratory)21/06/2016, 09:30At 17:48 UT on the 29th of March 2014, NOAA active region (AR) 12017 produced an X1 flare observed simultaneously by an unprecedented number of observatories. Among these were the Interface Region Imaging Spectrometer (IRIS) and Hinode’s Extreme Ultraviolet Imaging Spectrometer (EIS), joint observations from which provide an excellent opportunity to investigate the dynamics of the solar...Go to contribution page
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Jana Kasparova (Astronomical Institute of the CAS)21/06/2016, 09:50Using numerical RHD code Flarix we simulate the behaviour of MgII lines in the flaring chromosphere heated by electron beams. This contribution will focus on the role of partial redistribution, non-thermal collisional rates, and radiative losses. The role of different types of the temporal heating profiles, e.g. a long duration heating versus pulse heating will be assessed as well. The...Go to contribution page
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Arun Kumar Awasthi (Institute of Astronomy, University of Wroclaw)21/06/2016, 10:10The study of continuum enhancement during a flare is of immense interest owing to the fact that it represents significant fraction of the impulsive energy release and thus provides useful diagnostics of the energy deposition and emission processes in the photospheric and chromospheric heights. We study the spatial and temporal evolution of continuum enhancement (CE) and co-temporal...Go to contribution page
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Jaime de la Cruz Rodriguez (Stockholm University)21/06/2016, 11:15I will review the current state of non-LTE inversions and magnetic field inference in the solar chromosphere.Go to contribution page
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Tine Libbrecht (Institute for Solar Physics, Stockholm University)21/06/2016, 11:45Ellerman Bombs (EBs) are short-lived emission features observed in the wings of Balmer lines of hydrogen. So far, no distinct signature of EBs has been found in the He I λ10830 line, and observations of EBs in He I D3 have never been reported. We aim to study the signature of EBs in neutral helium triplet lines using SST/TRIPPEL raster scans, featuring the Hβ, He I D3 and He I λ10830...Go to contribution page
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Sanja Danilovic (Max Planck Institute for Solar System Research)21/06/2016, 12:05Recent SST observations have given a new definition of Ellerman bombs (EBs). They are short-lived flame-like features visible in the wings of Halpha, away from the disc center. EBs seem to be associated with a peculiar combination of signatures in different observables. Also, they could be placed on, energetically, a low end of the whole spectrum of events that might have the same physical...Go to contribution page
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Andres Asensio Ramos (Instituto de Astrofisica de Canarias)21/06/2016, 12:25Solar images obtained in the core of strong chromospheric lines show fibrils that appear to be tracing the magnetic field lines. They have been historically used as proxies of magnetic fields for many purposes. In this work we use a Bayesian hierarchical model to analyze several tens of thousands of pixels in spectro-polarimetric chromospheric images and compare the alignment between the...Go to contribution page
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