Principal Investigator:
Peter Hauschildt
, Hamburger Sternwarte, Universität Hamburg (Germany)
HPC Platform used:
Hazel Hen of HLRS
Local Project ID:
PP14112588
Understanding the light emitted by (magnetically) active cool stars (‘M dwarfs’) is a major challenge for astrophysics. In this project, scientists use their PHOENIX/3D code to simulate the light emitted by a ‘box’ inside the outer layers of an active M dwarf in detail. The temperatures and pressures inside the box are taken from an existing gas dynamics simulation (including magnetic field effects) by S. Wedemeyer (Oslo). The computational requirements of detailed non-equilibrium 3D radiative transfer simulations are staggering and require the largest supercomputers on Earth.
