62 citations · 624 across the 31 of their papers we have counts for
19 papers · 1 filter
Modeling the astrosphere of LHS~1140
K. Scherer, K. Herbst, N. E. Engelbrecht +3
The cosmic ray (CR) flux, as well as the hydrogen flux into the atmosphere of an exoplanet, can change the composition of the atmosphere. Here, we present the CR and hydrogen flux…
An exact analytical solution for the weakly magnetized flow around an axially symmetric paraboloid, with application to magnetosphere models
Jens Kleimann, Christian Röken
Rotationally symmetric bodies with longitudinal cross sections of parabolic shape are frequently used to model astrophysical objects, such as magnetospheres and other blunt objects…
Modelling O-star astrospheres with different relative speeds between the ISM and the star: 2D and 3D MHD model comparison
L. R. Baalmann, K. Scherer, J. Kleimann +3
Context. State of the art simulations of astrospheres are modelled using three-dimensional (3D) magnetohydrodynamics (MHD). An astrospheric interaction of a stellar wind (SW) with…
An Exact, Time-dependent Analytical Solution for the Magnetic Field in the Inner Heliosheath
Christian Röken, Jens Kleimann, Horst Fichtner
We derive an exact, time-dependent analytical magnetic field solution for the inner heliosheath, which satisfies both the induction equation of ideal magnetohydrodynamics in the li…
On the Diversity of M-Star Astrospheres and the Role of Galactic Cosmic Rays Within
Konstantin Herbst, Klaus Scherer, Stefan E. S. Ferreira +7
With upcoming missions such as the James Webb Space Telescope (JWST), the European Extremely Large Telescope (ELT), and the Atmospheric Remote-sensing Infrared Exoplanet Large-surv…
MHD-shock structures of astrospheres: Cephei-like astrospheres
K. Scherer, L. R. Baalmann, H. Fichtner +5
The interpretation of recent observations of bow shocks around O-stars and the creation of corresponding models require a detailed understanding of the associated (magneto-)hydrody…
Skymaps of observables of three-dimensional MHD astrosphere models
L. R. Baalmann, K. Scherer, H. Fichtner +3
Three-dimensional models of astrospheres have recently become of interest. However, comparisons between these models and observations are non-trivial because of the two-dimensional…
The interaction of multiple stellar winds in stellar clusters: potential flow
Klaus Scherer, Alexander Noack, Jens Kleimann +2
While several studies have investigated large-scale cluster winds resulting from an intra-cluster interaction of multiple stellar winds, as yet they have not provided details of th…
An Improved Analytical Model of the Local Interstellar Magnetic Field: The Extension to Compressibility
J. Kleimann, C. Röken, H. Fichtner
A previously published analytical magnetohydrodynamic model for the local interstellar magnetic field in the vicinity of the heliopause (Röken et al. 2015) is extended from incompr…
Generalized multi-polytropic Rankine-Hugoniot relations and the entropy condition
Klaus Scherer, Horst Fichtner, Hans Jörg Fahr +2
The study aims at a derivation of generalized \RH relations, especially that for the entropy, for the case of different upstream/downstream polytropic indices and their implication…
A generalized two-component model of solar wind turbulence and ab initio diffusion mean free paths and drift lengthscales of cosmic rays
Tobias Wiengarten, Sean Oughton, Eugene Engelbrecht +3
We extend a two-component model for the evolution of fluctuations in the solar wind plasma so that it is fully three-dimensional (3D) and also coupled self-consistently to the larg…
Shock structures of astrospheres
Klaus Scherer, Horst Fichtner, Jens Kleimann +3
The interaction between a supersonic stellar wind and a (super-)sonic interstellar wind has recently been viewed with new interest. We here first give an overview of the modeling,…
Toward more realistic analytic models of the heliotail: Incorporating magnetic flattening via distortion flows
Jens Kleimann, Christian Röken, Horst Fichtner +1
Both physical arguments and simulations of the global heliosphere indicate that the tailward heliopause is flattened considerably in the direction perpendicular to both the incomin…
Implementing turbulence transport in the CRONOS framework and application to the propagation of CMEs
Tobias Wiengarten, Horst Fichtner, Jens Kleimann +1
We present the implementation of turbulence transport equations in addition to the Reynolds-averaged MHD equations within the Cronos framework. The model is validated by comparison…
An exact analytical solution for the interstellar magnetic field in the vicinity of the heliosphere
Christian Röken, Jens Kleimann, Horst Fichtner
An analytical representation of the interstellar magnetic field in the vicinity of the heliosphere is derived. The three-dimensional field structure close to the heliopause is calc…
A novel code for numerical 3-D MHD studies of CME expansion
Jens Kleimann, Andreas Kopp, Horst Fichtner +1
A recent third-order, essentially non-oscillatory central scheme to advance the equations of single-fluid magnetohydrodynamics (MHD) in time has been implemented into a new numeric…
Non-ideal MHD Properties of Magnetic Flux Tubes in the Solar Photosphere
Jens Kleimann, Gunnar Hornig
Magnetic flux tubes reaching from the solar convective zone into the chromosphere have to pass through the relatively cool, and therefore non-ideal (i.e. resistive) photospheric re…
4pi Models of CMEs and ICMEs
Jens Kleimann
Coronal mass ejections (CMEs), which dynamically connect the solar surface to the far reaches of interplanetary space, represent a major anifestation of solar activity. They are no…
Magnetic clouds in the solar wind: A numerical assessment study of analytical models
G. Dalakishvili, J. Kleimann, H. Fichtner +1
Magnetic clouds (MCs) are "magnetized plasma clouds" moving in the solar wind. MCs transport magnetic flux and helicity away from the Sun. These structures are not stationary but f…