|
Coronal-Dynamics: Understanding the structure and dynamics of the corona
Theory group
Cool stars like our Sun are surrounded by a million Kelvin hot outer
atmosphere, the corona. It is still puzzling what sustains its high
temperature, being 100 to 1000 times hotter than the stellar surface.
Being related to (changes of) the magnetic field, we can expect the
heating mechanism to change the structure of the corona, to drive plasma
flows, and to induce wave phenomena. On the Sun we can observe this
dynamic evolution of the corona in detail, especially through spectroscopy
and imaging at extreme ultraviolet and X-ray wavelengths.
Project description
Coronal-Dynamics home page
|
| |
|
|
Sun-Climate: Solar variability and climate
Theory group
Radiation from the Sun makes Earth a habitable planet. Fluctuations in
the solar radiative output are therefore likely to affect the climate
on Earth, but establishing both how the output of the Sun varies and how
such variations influence Earth's climate have proved tricky. Increased
amounts of data from the Sun and about the climate on Earth over recent
years means that rapid progress is being made. This work is aimed at
understanding solar variability and the Sun's influence on the Earths'
climate.
Project description
Sun-Climate home page
|
| |
|
|
CSI: Coronal Spectroscopy and Imaging
Data Analysis
The group studies physical processes in the solar chromosphere,
transition region and corona, thereby applying both observational
techniques and theoretical modelling. The upper solar atmosphere
is best observed in the wavelength ranges of the far and extreme
ultraviolet and soft X-rays, emissions that are only accessible
from space. Our research aims at describing and understanding the
fundamental plasma processes at all scales in the upper solar
atmosphere and addresses in particular the unsolved problems of
coronal heating and solar wind acceleration. We also study atomic
radiation processes, ionic excitation and de-excitation, radiation
transport and wave-particle interactions.
Project description
|
| |
|
|
SoCo3D: Solar Corona in 3D
Theory group
The magnetic field couples the solar interior with the photosphere and
corona where it drives heating processes and eruptive phenomena like
flares and coronal mass ejections. We developed sophisticated computer-codes
to model the coronal magnetic field and plasma by nonlinear and self-consistent
extrapolation techniques, stereoscopy and tomography.
Project description
SoCo3D home page
|
| |
|
|
Solar-MHD: Solar and stellar magnetohydrodynamics
Theory group
Magnetohydrodynamics (MHD) describes the dynamical interaction between
flows and magnetic fields in a collisionally dominated plasma. The work
of the MHD group at MPAe is mainly concerned with MHD processes in the
interior and atmosphere of the Sun and other stars. Using large-scale
numerical simulations and analytical tools, this work aims at
understanding the origin of solar and stellar magnetism as well as its
rich variety of manifestations in the form of magnetic activity.
Project description
Solar-MHD home page
|
| |
|
|
Solar-Plasma: Solar Wind Particles and Fields
Data analysis and theory group
The group is mainly engaged in theory and modelling of the solar
corona and solar wind, with emphasis on plasma kinetics and
magnetohydrodynamic (MHD) turbulence. The solar research aims at
understanding basic plasma processes at all scales in the solar
corona, especially in the transition region, and addresses the
fundamental problem of coronal heating by plasma waves and
small-scale magnetic activity. The solar wind research focuses
on MHD turbulence and wave-particle interactions.
Project description
|
| |
|
|
Plasma-Simulations: Theory and simulation of solar system plasmas
Theory group
The main emphasis of the research work in the group is put on the
energy release in the Universe by magnetic reconnection and on the
resulting turbulence, structure formation, plasma heating and particle
acceleration to high energies. Applications are magnetic 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 particle acceleration. The research methods are kinetic
(Vlasov- and PIC-code) simulations as well as combined kinetic-MHD
plasma simulations, developed in the group. Starting from
heliosphysical plasma processes conclusions are drawn als for
galactic and extragalactic plasma processes like jets out of active
galactic nuclei or the interaction of extrasolar planets with their
stars.
Project description
|
| |
|
|
SLAM: Solar Lower Atmosphere and Magnetism
Data Analysis
Imaging and spectroscopy of the Sun in the near UV, visible and
near IR: High-resolution solar imaging using phase diversity image
reconstruction techniques and High-precision spectro-polarimetry
(Zeeman polarimetry and Hanle diagnostics of scattering polarization).
Project description
SLAM home page
|
| |
|
|
Solar-Orbiter: High-Resolution Mission to the Sun and Inner Helisphere
Planned Launch: 2017
The scientific rationale of the Solar Orbiter (SO) is to provide, at
high spatial and temporal resolution, multi-wavelength observations
of the solar atmosphere and comprehensive in-situ measurements of the
unexplored inner heliosphere. Solar Orbiter is now proposed for ESA's
Cosmic Vision programme.
Participation:
PHI: Polarimetric and Helioseismic Imager, SPICE: Spectral Imaging of the Coronal Environment, EUI: Extreme Ultraviolet Imager, METIS-ICOR: Multi Element Telescope for Imaging and Spectroscopy
Project description
Solar-Orbiter home page
|
| |
|
|
Sunrise: A balloon-borne solar telescope
Planned first flight: 2009
The Sunrise project aims at high-resolution spectro-polarimetric
observations of the solar atmosphere on the intrinsic spatial scale of
its magnetic structure. The Sunrise telescope with 1 m aperture and its
instruments will provide spectra and images resolving spatial scales
down to 35 km on the Sun. The main scientific goal of the mission is to
understand the formation of magnetic structures in the solar atmosphere
and to study their interaction with the convective plasma flows.
Project description
Sunrise home page
|
| |
|
|
STEREO: The Solar TErrestrial RElations Observatory
Planned Launch: August 2006
STEREO is a NASA mission designed to make the first 3D observations of
the Sun and inner Heliosphere to help unveil the origin, evolution and
interplanetary consequences of coronal mass ejections.
Participation:
SECCHI: EUV imager and white-light coronagraphs, IMPACT: Solar energetic particle package
Project description
STEREO home page
|
| |
|
|
SOHO: The Solar and Heliospheric Observatory
Launch: December 2, 1995
SOHO is designed to study the internal structure of the Sun,
its extensive outer atmosphere and the origin of the solar wind,
the stream of highly ionized gas that blows continuously outward
through the Solar System. The view of the Sun is achieved by
operating SOHO from a permanent vantage point 1.5 million kilometers
sunward of the Earth in a halo orbit around the L1 Lagrangian point.
Participation:
SUMER: UV spectrometer, LASCO: Coronagraph, CELIAS: Particle instrument
Project description
SOHO home page
|
| |
|
|
ULYSSES: The solar polar mission
Launch: October 6, 1990
A joint project between NASA and the European Space Agency, Ulysses
was carried into Earth orbit aboard the Space Shuttle Discovery and
propelled toward Jupiter, where the giant planet's gravity helped
direct the craft's flight path into an unusual orbit around the Sun
(first spacecraft to leave the ecliptic plane). It has since made
several orbital passes of the Sun's north and south poles.
Participation:
EPAC: Energetic PArticles Composition Instrument, GAS: Neutral Gas Instrument, SWICS: Particle Instrument
Project description
ULYSSES home page
|
| |
|
|
HELIOS: German-American spacecraft orbiting the sun
HELIOS 1: 1974 - 1986, HELIOS 2: 1976-1980
Helios 1 and Helios 2 were a pair of deep space probes developed in
Germany in a cooperative program with NASA.
Participation:
E1: Plasma instrument, E8: Particle instrument
Project description
|
