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SUMMARY:Formation of MgII h&k spectra in an enhanced network region simula
 ted with MURaM
DTSTART;VALUE=DATE-TIME:20230511T071500Z
DTEND;VALUE=DATE-TIME:20230511T073000Z
DTSTAMP;VALUE=DATE-TIME:20240704T115655Z
UID:indico-contribution-336@meetings.aip.de
DESCRIPTION:Speakers: Patrick Ondratschek (Max Planck Institute for Solar 
 System Research)\nUnderstanding the physical processes in the solar chromo
 sphere requires comprehensive models which can be compared to observations
 . These models include the treatment of magnetic fields\, heat conduction 
 and radiative transfer (RT). However\, usually models fail to reproduce ob
 served properties of chromospheric spectral lines. The MgII h&k lines form
  in the middle to upper chromosphere and are observed by the IRIS satellit
 e mission with high precision. The forward modeled spectral lines appear o
 n average to have too narrow line widths and larger peak asymmetries than 
 the observations.\n We use the recently developed chromospheric extension 
 of the radiative MHD code MURaM to simulate an enhanced network (EN) regio
 n. From the resulting modeled atmospheres we use the RT codes RH1.5D and M
 ulti3D to synthesize the MgII h&k lines in 1D and 3D RT. We find that the 
 line width as well as the peak separations from the forward modeled spectr
 a are on average larger and in better agreement to observations. We discus
 s the physical properties such as velocity gradients and density stratific
 ation in the chromosphere of the modeled atmosphere that lead to the impro
 ved synthetic spectral profiles.\n\nhttps://meetings.aip.de/event/24/contr
 ibutions/336/
LOCATION:Haus H\, Telegrafenberg
URL:https://meetings.aip.de/event/24/contributions/336/
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