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Mats Carlsson (Institute of Theoretical Astrophysics, University of Oslo)22/06/2016, 09:00The chromosphere is arguably the most difficult and least understood domain of solar physics. All at once it represents the transition from optically thick to thin radiation escape, from gas-pressure domination to magnetic-pressure domination, from neutral to ionised state, from MHD to plasma physics, and from near-equilibrium (LTE") to non-equilibrium conditions. The...Go to contribution page
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Vanessa Polito (University of Cambridge)22/06/2016, 09:30The intensity of the OIV and SIV intercombination lines around 1400 Å observed with the Interface Region Imaging Spectrograph (IRIS) provide a useful tool to diagnose the electron number density in the solar transition region plasma. We measure the electron density in a variety of solar features, including a loop and a bright point in the AR NOAA 12356 and at the ribbons of the...Go to contribution page
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Andrii Sukhorukov (Institutet för solfysik, Stockholms universitet)22/06/2016, 09:50We studied the formation of the most practically important resonance lines such as H I Ly-a, Mg II k&h, and Ca II K&H in the chromosphere using 3D MHD snapshots produced by the Bifrost numerical code. For this purpose, we implemented effects of partial redistribution (PRD) using the hybrid approximation of Leenaarts et al. (2012) into our radiative transfer code. We discuss some technical...Go to contribution page
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Haruhisa Iijima (Institute for Space-Earth Environmental Research (ISEE), Nagoya University)22/06/2016, 10:10A three-dimensional simulation by the Tokyo code (tentative name) is presented to investigate the effect of three-dimensionality on the scale of chromospheric jets and the dependence on the photospheric magnetic field structure. We newly develop a numerical code for the radiation magnetohydrodynamic modeling of solar atmosphere. The code includes the effect of non-local radiative transfer...Go to contribution page
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Hardi Peter (MPI for Solar System Research)22/06/2016, 11:15There is an everlasting mass cycle between the chromosphere and the upper atmosphere, the transition region and the corona. Many suggestions have been made on the nature of this mass cycle, from handwaving arguments to 3D MHD models. However, each of these suggestions has its problems and it is unclear what really governs the mass exchange. For example the transition region emission in...Go to contribution page
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Tanmoy Samanta (Indian Institute of Astrophysics)22/06/2016, 11:45The solar chromosphere and transition region plays an important role in understanding the interaction between the relatively cool photospheric plasma and the hot multi-million degree corona. It is only beginning to be understood where and how the required energy is generated, transported and dissipated. It appears that the chromosphere and transition region plays a key role in the process....Go to contribution page
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Tiago M. D. Pereira (University of Oslo)22/06/2016, 12:05Low-lying loops have been observed by IRIS at the solar limb in transition region temperatures. It has been suggested that these loops constitute a connection between the corona and transition region, previously known as unresolved fine structure (UFS). In this work we make use of coordinated observations between IRIS and the Swedish 1-m Solar Telescope to study these low-lying loops. We...Go to contribution page
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Pia Zacharias (University of Oslo)22/06/2016, 12:25Observations of solar transition region emission lines reveal the presence of redshifts up to temperatures of about 300,000 K and blueshifts for higher temperatures. The apparent large downward flows in the lower transition region would lead to an emptying of the corona, in contrast to what is being observed, thus some mechanism must be responsible for maintaining the mass balance between...Go to contribution page
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