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SUMMARY:Photospheric MHD simulations: From sub-granular scales to active r
 egions
DTSTART;VALUE=DATE-TIME:20230509T070000Z
DTEND;VALUE=DATE-TIME:20230509T073000Z
DTSTAMP;VALUE=DATE-TIME:20240704T115653Z
UID:indico-contribution-362@meetings.aip.de
DESCRIPTION:Speakers: Matthias Rempel (High Altitude Observatory\, Nationa
 l Center for Atmospheric Research)\nMore than 20 years ago most photospher
 ic MHD simulations focused primarily on small patches of granulation with 
 moderate numerical resolution. Over the past 2 decades advances in computi
 ng infrastructure have enabled photospheric MHD simulations to cover most 
 magnetic environments from quiet Sun to active Sun. In this talk I review 
 these recent developments and focus primarily on simulations that cover th
 e extreme ends of the spectrum: (1) Small-scale dynamo simulations of quie
 t Sun magnetism and (2) Simulations of active region scales. (1) Recent re
 search (observations and modeling) supports the view that the origin of sm
 all-scale magnetism is mostly due to a small-scale dynamo that operates in
 dependently from the large-scale dynamo responsible for the solar cycle. R
 ecent simulations have shown that the saturation field strength and struct
 ure of the resulting magnetic field in the photosphere depend critically o
 n the contributions from deep and shallow recirculation within the strongl
 y stratified convection zone. Therefore\, the small-scale dynamo is not re
 stricted to the photosphere and involves a wide range of scales. Recent re
 search suggests that small-scale magnetic fields may play a critical role 
 for convection zone dynamics. Outstanding questions concern the role of th
 e magnetic Prandtl number\, which will require in the future simulations w
 ith better resolution (\n\nhttps://meetings.aip.de/event/24/contributions/
 362/
LOCATION:Haus H\, Telegrafenberg
URL:https://meetings.aip.de/event/24/contributions/362/
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