The dynamical chromosphere and its role in energy transfer through the solar atmosphere: Results from IRIS

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An RAS Specialist Discussion Meeting organised by Louise Harra (MSSL/UCL)* and Alan Hood (St. Andrews)*Contact: lkh AT chromosphere is an extremely complex and very dynamical part of the solar atmosphere. Presently, it is unclear how this region physically interacts with the lower photosphere, upper transition region and corona. The NASA IRIS mission was launched in 2013 with the explicit goal of exploring the chromosphere spectroscopically, with high spatial, temporal and spectral resolution. IRIS has been observing alongside existing missions sich as Hinode and SDO, providing unprecedented coverage throughout the solar atmosphere. The purpose of this discussion meeting is to:

  1. highlight the first results from the IRIS mission that are showing incredible complexity in the spectral profiles,
  2. link IRIS observations to those in the photosphere and corona,
  3. use theory and simulations to advance our physical understanding of the energy transfers between all of these layers.

Full details are available from:
10:30-10:55 (invited) Mats Carlsson, University of OsloChromospheric Modelling11:00-11:15 Richard Morton, Northumbria UniversityWhat Hi-C told us about the structure and dynamics of an AR Transition Region11:20-11:35 Jaroslav Dudik, University of CambridgeOn the formation of IRIS transition-region lines in non-Maxwellian conditions11:40-11:55 Ineke De Moortel, University of St. AndrewsJoint SDO/AIA and IRIS Observations of Propagating Coronal Disturbances12:00-12:15 Philip Judge, HAO, National Center for Atmospheric ResearchUltra-high cadence observations reveal plasma sheets in the solar chromosphere12:20-12:35 Sarah Matthews, MSSL, University College LondonProbing Energy Release & Transport in Flares - New insights from IRIS and Hinode12:40-13:40 Lunch13:40-14:05 (invited) Bart De Pontieu, Lockheed Martin Solar & Astrophysics LaboratoryTBA14:10-14:25 Graham Kerr, University of GlasgowMg II h & k Line Emission During a Solar Flare14:30-14:45 Peter Levens, University of GlasgowAre tornadoes different from prominence legs?14:50-15:05 Vanessa Polito, University of CambridgeJoint High Temperature Observation of a small C6.5 Solar Flare with IRIS/EIS/AIA15:10-15:25 Vasilis Archontis, University of St. AndrewsClusters of small eruptive flares produced by magnetic reconnection in the solar atmospherePosters:Brigitte Schmieder, Observatoire de ParisEmergence observed by the IRIS spectrometerAndrew Hillier, University of CambridgeA numerical investigation into the dopplershift profiles of prominence dynamics