Ferreira:
   -- (M)HD of astrospheres: significance of cooling functions and ISM
   -- CRs in astrospheres
   -- supernova evolution with/without cavity
   -- CRs in supernova cavities

    Q: (spatially) 1D simulations sufficient?
    Q: observational discrimination between cooling models?
    Q: significance of non-equilibrium radiation transport?

Scherer:
   -- interaction of multiple astrospheres 
   -- regularized kappa-distributions
   -- moving Str\"omgren spheres
   -- cosmic ray anisotropies
   -- astrosphere interaction with ISM: structure of discontinuities
   -- computation of observables

    Q: artifacts in the computations of observables?
    Q: how to obtain knowledge about ISM paramaters? 

Kleimann:
   -- Sun's cosmic ray shadow
   -- models of the LISM B-field
   -- Galaxy's B-field: solenoidality corrected at inner and outer radius
                        removal of "kinks" in fieldlines at z=0
   -- interaction of multiple astrospheres: stellar cluster winds

    Q: discrimination via current density distribution in and near z=0 ?

Heber:
   -- instrument modeling and instrument development
   -- GCR modulation and propagation: new AMS 02 
   -- impact on atmosphere
   -- dosimetry

    Q: symmetry of charge dependence of e-/e+ in dependence on their spectra

Herbst:
   -- stellar particle environment (G,K,M)
   -- influence on (exo)planetary habitability

    Q: cross check via correlation of X-ray flux & mass loss rate

Wolf: 
   -- from clouds to disks: magnetic fields
   -- planet-disk interaction
   -- impact of magnetic fields

    Q: column depths for CRs? 
    Q: effect of CRs significant? - unclear
    Q: inclusion via kinetic transport eq. (test part.) or hydrodynamically?

Dettmar:
   -- CRs in galactic halos
   -- B-fields and CRs in starforming disk galaxies
   -- ionisation of halo gas via CRs

    Q: equipartition in halo or only in disk ISM?
    Q: Cartesian-shaped outflow consequence of angular momentum issue?

Letarte:
   -- stellar pulsations (of mostly Ap and Am stars) 
   -- pulsations = "garbage" for the planet hunters:-)
   -- astrophotography: public outreach!

    Q: discrimination of exoplanet-induced variations and pulsations? 
    Q: input to webpage?

Venter:
   -- pulsar system queations: electrodynamics, pair plasma physics, 
      relativistic winds, part. acc., mag. reconection geometry, beaming, evol. 
   -- several shocks: termination shock, PWN shock, reverse shock, bow shock?
   -- conversion from mag. to part. energy (sigma problem)
   -- CTA: higher resolution
   -- "spider binaries" MSPs in close binaries
   -- white-dwarf pulsar

    Q: relativistic MHD?
    Q: particle motion along the shock or astropause?
    Q: MHD for e+/e- plasmas?

Dresing:
   -- solar energetic particles
   -- multi-spacecraft observations of widespread events
   -- anisotropy over broad longitude range implies anisotropy close to the Sun

    Q: anisotropy built-up along the way? -- not possible

Strauss:
   -- SEP modelling with detailed turbulence models
   -- CR measurements via neutron monitors
   -- aviation dosimetry

    Q: hardware equipment supported by DFG?
    Q: hardware development suported by DFG?

Wimmer-Schweingruber: 
   -- origin of the solar wind
   -- transport of suprathermal particles
   -- dosimetry on the Moon (CR surface interaction)
   -- dosimetry on Mars (multipoint measurements!)

    Q: Solar Orbiter & Parker Solar Probe active during IRTG

Engelbrecht/Moloto:
   -- turbulence, diffusion, and cosmic rays
   -- LH, RH waves, electron transport
   -- PUI wave generation & electron MFP
   -- drift reduction 
   -- time-dependent modulation

    Q: PUI-generated waves heat SW, so not available for reduction of e-MFP? 
    Q: non-axisymmetric turbulence --> perpendicular diffusion anisotropic?
    Q: How about other species (i.e. other than Jovians & protons)

Grauer:
   -- synthetic turbulence
   -- Kramers-Moyal expansion
    
    Q: Kr-Mol exp. allows for intermittency, i.e. generally for inhomog. backg.?
    Q: turbulent field can be different from velocity field?
    Q: She-Leveque-like models corresponds to subdiffusion?
    
Fichtner:
   -- MHD turbulence evolution
   -- nonlinear diffusion
   -- kinetic solar/stellar wind 
   -- full-orbit simulations

    Q: Is mirroring observed in the LISM? 

  ****************************************************************************


To Do's:
========

 -- list of theses topics: topic and an explanatory sentence
 -- potential respective foreign collaborators
 -- missions during funding period of IRTG/access to facilities
 -- list of potential reviewers (DFG is sometimes asking)