SH038-03
Dynamics and thermal structure in the quiet Sun seen by SPICE

Monday, 14 December 2020: 05:38
Virtual
Hardi Peter1, Regina Aznar Cuadrado2, Udo Schühle2, Luca Teriaca2, F Auchere3, Mats Carlsson4, Andrzej Fludra5, Don Hassler6, Eric Buchlin3, Stéphane Caminade3, Martin Caldwell5, Craig DeForest6, Terje Fredvik4, Louise K Harra7, Miho Janvier3, Therese Ann Kucera8, Alessandra S Giunta5, Tim Grundy5, Daniel Müller9, Susanna Parenti10, Werner K Schmutz7, Sunil Sidher5, William T Thompson11, David Williams12 and Peter R Young8, (1)Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany, (2)Max Planck Institute for Solar System Research, Göttingen, Germany, (3)Université Paris-Saclay, CNRS, Institut d'Astrophysique Spatiale, Orsay, France, (4)University of Oslo, Institute of Theoretical Astrophysics, Oslo, Norway, (5)RAL Space, STFC Rutherford Appleton Laboratory, Didcot, United Kingdom, (6)Southwest Research Institute, Boulder, CO, United States, (7)Physikalisch-Meteorologisches Observatorium Davos, World Radiation Center, Davos Dorf, Switzerland, (8)NASA Goddard Space Flight Center, Greenbelt, MD, United States, (9)European Space Agency, ESTEC, Noordwijk, Netherlands, (10)Institut d'Astrophysique de Paris, Paris, France, (11)ADNET Systems Inc., NASA Goddard Space Flight Center, Greenbelt, MD, United States, (12)European Space Agency, ESAC, Villanueva De La Cañada, Madrid, Spain
Recorded Presentation
Abstract:
We will present some of the early data of the Spectral Imaging of the Coronal Environment (SPICE) instrument on Solar Orbiter. One of the unique features of SPICE is its capability to record a wide range of wavelengths in the extreme UV with the possibility to record spectral lines giving access to a continuous plasma temperature range from 10.000 K to well above 1 MK. The data taken so far were for commissioning purposes and they can be used for a preliminary evaluation of the science performance of the instrument. Here we will concentrate on sample spectra covering the whole wavelength region and on the early raster maps acquired in bright lines in the quiet Sun close to disk center. Looking at different quiet Sun features we investigate the thermal structure of the atmosphere and flow structures. For this we apply fits to the spectral profiles and check the performance in terms of Doppler shifts and line widths to retrieve the structure of the network in terms of dynamics. While the amount of data available so far is limited, we will have a first look on how quiet Sun plasma responds to heating events. For this, we will compare spectral lines forming at different temperatures recorded at strictly the same time.
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