Homepage of the Plasma Simulations Group

Contact

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Prof. Dr. Joerg Buechner
Wissenschaftler
Phone:+49 551 384 979 - 295

Secretary

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Andrea Vogt
Sekretariat
Phone:+49 551 384 979 - 278
Email:vogta@...

Members of the Group

Staff scientists:
Jörg Büchner
Neeraj Jain

Postdocs:
Patricio Munoz

TSSSP Group 2014:<br />Patrick Kilian, J&ouml;rg B&uuml;chner, Jan Skala, Neeraj Jain, Fabien Widmer, Patricio Munoz, Suzana de Souza, Xiaowei Zhou and Sijie Yu Zoom Image
TSSSP Group 2014:
Patrick Kilian, Jörg Büchner, Jan Skala, Neeraj Jain, Fabien Widmer, Patricio Munoz, Suzana de Souza, Xiaowei Zhou and Sijie Yu [less]

Visiting scientists

Prof. Dr. A. Otto, U.S.A.

Prof. Dr. G. Choe, Korea

Former Members of the group

E. Adamson
M. Barta
N. Elkina
J. Guo (PHD in 2010)
S. Javadi (PHD in 2010)
K.W. Lee (PHD in 2008)
J.-P. Kuska († 2009)
B. Nikutowski
S. Preusse (PHD in 2006)
J. C. Santos (PHD in 2008)
I. Silin (PHD in 2004)
H. Wiechen († 2008)
Th. Wiegelmann
S. Yang (PHD 2009)

Projects

Onngoing projects the TSSP group is involved in:

Project “Magnetic reconnection in space and laboratory” within the Max-Planck-Princeton Center for Plasma Physics

CRC 963 "Astrophysical Flow Instabilities and Turbulence"
Sub-project A2 of the CRC 963 „From solar to heliospheric flows and instabilities
Sub-project A15 of the CRC 963 „Simulations of reconnection and dynamo action in turbulent plasma flows

Space Projects:
CLUSTER
INTERBALL
STEREO
SDO

Future projects with TSSSP involvement:
Solar Orbiter - EUI

Planned projects with TSSSP involvement:
Plato

 

TSSSP: Theory and Simulation of Solar System Plasmas

TSSSP: Theory and Simulation of Solar System Plasmas

The Theory group TSSSP investigates plasma processes of the energy release in the Universe by magnetic reconnection, turbulence and its consequences, structure formation, plasma heating and particle acceleration to high energies. Examples are stellar and solar eruptions, magnetic storms and substorms in planetary magnetospheres, the heating of the solar corona, e.g. of EUV and X-ray Bright Points, solar flares, coronal mass ejections and the acceleration of the solar wind, of solar plasma- and particle streams with consequences  for the Earth ("Space Weather"). The methods applied are kinetic as well as fluid plasma theories and simulation methods. As an example Figure 1 shows the result of simulations using our 3D MHD code LINMOD3D –The structure of three-dimensional magnetic reconnection in the solar  atmosphere in case of quadrupolar magnetic fields.

<p>Three-dimensional magnetic reconnection in the solar atmosphere: quadrupolar magnetic fields cause hot spots in the corona (temperature: millions of Kelvin, more than hundert times than at the solar surface).</p>

Three-dimensional magnetic reconnection in the solar atmosphere: quadrupolar magnetic fields cause hot spots in the corona (temperature: millions of Kelvin, more than hundert times than at the solar surface).

Since turbulence is always present in space plasmas over many scale length the group also deals with microscopic plasma-kinetic simulations. Figure 2 shows the simulated magnetic field resulting from plasma kinetic numerical simulations of reconnection in the solar corona.

<p>Magnetic reconnection and turbulence are closely related to each other. The figure shows the magnetic field resulting from plasma kinetic numerical simulations of reconnection in the solar corona.</p>

Magnetic reconnection and turbulence are closely related to each other. The figure shows the magnetic field resulting from plasma kinetic numerical simulations of reconnection in the solar corona.

The theoretical investigations of the group are carried out in close relation with observational programs. Especially important is the collaboration of the group with laboratory plasma physicists in the framework of the Max-Planck-Princeton Center for Plasma Physics since it allows to verify the theories of space plasma phenomena at Earth. Starting from plasma processes in the solar system conclusions are drawn also for galactic and extragalactic plasma processes like the interaction of extrasolar planets  with their stars. For this sake we collaborate with astrophysicists from the universities of Göttingen and Braunschweig in the framework of the Coordinated research center (CRC) 963 “Astrophysical Flow Instabilities and Turbulence”.

 
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