BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//CERN//INDICO//EN
BEGIN:VEVENT
SUMMARY:Comprehensive simulation of a solar prominence with MURaM
DTSTART;VALUE=DATE-TIME:20230510T130500Z
DTEND;VALUE=DATE-TIME:20230510T132000Z
DTSTAMP;VALUE=DATE-TIME:20240704T115655Z
UID:indico-contribution-328@meetings.aip.de
DESCRIPTION:Speakers: Lisa-Marie Zessner (Max Planck Institute for Solar S
 ystem Research)\nSolar prominences consist of cool and dense plasma that i
 s suspended in the corona\, surrounded by hotter and less dense coronal ma
 terial. As predecessors of coronal mass ejections\, solar prominences are 
 important drivers of space weather\, but their exact formation mechanism i
 s still unknown. We use the radiative magnetohydrodynamic code MURaM to si
 mulate the formation and dynamics of a prominence in the solar atmosphere.
  MURaM includes the relevant physical processes to realistically simulate 
 the solar photosphere\, chromosphere and corona.\n\nWe create a stable dip
 ped magnetic field configuration in a 3D box of size 80 x 30 x 10 Mm and l
 et it evolve. In the course of the simulation\, a dense plasma seed ejecte
 d from the chromosphere randomly settles into a magnetic dip and is cooled
  by radiative losses. The resulting pressure drop drives a strong flow of 
 plasma into the feature and builds up a cool\, long-lasting structure in t
 he solar corona. This prominence is very dynamic but stable due to the sta
 bility of the underlying magnetic field. Its properties and dynamics are c
 omparable to certain observations of real prominences. In this contributio
 n\, we present the formation mechanism and properties of the simulated pro
 minence.\n\nhttps://meetings.aip.de/event/24/contributions/328/
LOCATION:Haus H\, Telegrafenberg
URL:https://meetings.aip.de/event/24/contributions/328/
END:VEVENT
END:VCALENDAR