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DTSTAMP:20190719T085744Z
LOCATION:HG F 30
DTSTART;TZID=Europe/Stockholm:20190614T103000
DTEND;TZID=Europe/Stockholm:20190614T110000
UID:submissions.pasc-conference.org_PASC19_sess122_msa285@linklings.com
SUMMARY:Computational Challenges in Lagrangian Simulations of Magnetised A
 strophysical Fluids
DESCRIPTION:Minisymposium\nComputer Science and Applied Mathematics, Physi
 cs\n\nComputational Challenges in Lagrangian Simulations of Magnetised Ast
 rophysical Fluids\n\nMayer, Deng\n\nMagnetohydrodynamical instabilities pl
 ay an important role in a variety of astrophysical flows. In astrophysical
  disks they are occurring along with other complex processes, often in the
  presence of self-gravity, radiation and supersonic conditions. Lagrangian
  codes are very well suited to treat these highly dynamical situations but
  classical implementations of e.g. SPH are affected by particle noise whic
 h prevent resolving instabilities such as the magneto-rotational instabili
 ty (MRI). Evolution of the SPH method such as the meshless finite mass met
 hod (MFM) offer a way forward beyond such limitations. However, I will sho
 w how, even in these new methods, computational speed and scalability are 
 another limitation relative to Eulerian grid-based methods. The SPH neighb
 or search is a big culprit in the latter context. Strategies for Exascale,
  such as those developed in the SPH-EXA PASC project, will be highly benef
 icial to make major steps forward.
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