An exact, time-dependent analytical solution for the magnetic field in the inner heliosheath

@article{Rken2021AnET,
  title={An exact, time-dependent analytical solution for the magnetic field in the inner heliosheath},
  author={Christian R{\"o}ken and Jens Kleimann and Horst Fichtner},
  journal={Journal of Physics A: Mathematical and Theoretical},
  year={2021},
  volume={55}
}
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 limit of infinite electric conductivity and the magnetic divergence constraint. To this end, we assume that the magnetic field is frozen into a plasma flow resembling the characteristic interaction of the solar wind with the local interstellar medium. Furthermore, we make use of the ideal Ohm’s law for the magnetic… 

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References

SHOWING 1-10 OF 30 REFERENCES

TOWARD MORE REALISTIC ANALYTIC MODELS OF THE HELIOTAIL: INCORPORATING MAGNETIC FLATTENING VIA DISTORTION FLOWS

Both physical arguments and simulations of the global heliosphere indicate that the tailward heliopause is flattened considerably in the direction perpendicular to both the incoming flow and the

An Improved Analytical Model of the Local Interstellar Magnetic Field: The Extension to Compressibility

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 incompressible to

Modeling the Plasma Flow in the Inner Heliosheath with a Spatially Varying Compression Ratio

We examine a semi-analytical non-magnetic model of the termination shock location previously developed by Exarhos & Moussas. In their study, the plasma flow beyond the shock is considered

AN EXACT ANALYTICAL SOLUTION FOR THE INTERSTELLAR MAGNETIC FIELD IN THE VICINITY OF THE HELIOSPHERE

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 calculated as a

DRAPING OF THE INTERSTELLAR MAGNETIC FIELD OVER THE HELIOPAUSE: A PASSIVE FIELD MODEL

As the local interstellar plasma flows past our heliosphere, it is slowed and deflected around the magnetic obstacle of the heliopause. The interstellar magnetic field, frozen into this plasma, then

Three-dimensional Features of the Outer Heliosphere Due to Coupling between the Interstellar and Heliospheric Magnetic Field. V. The Bow Wave, Heliospheric Boundary Layer, Instabilities, and Magnetic Reconnection

The heliosphere is formed due to interaction between the solar wind (SW) and local interstellar medium (LISM). The shape and position of the heliospheric boundary, the heliopause, in space depend on

A MODEL OF THE HELIOSPHERE WITH JETS

An analytic model of the heliosheath (HS) between the termination shock (TS) and the heliopause (HP) is developed in the limit in which the interstellar flow and magnetic field are neglected. The

Global structure of the heliosphere: 3D kinetic-MHD model and the interpretation of spacecraft data

This paper is a brief overview of research into the interaction between the solar wind and local interstellar medium. This interaction determines the global structure of the heliosphere (the region

THE EFFECT OF NEW INTERSTELLAR MEDIUM PARAMETERS ON THE HELIOSPHERE AND ENERGETIC NEUTRAL ATOMS FROM THE INTERSTELLAR BOUNDARY

We present new results from three-dimensional simulations of the solar wind interaction with the local interstellar medium (LISM) using recent observations by NASA's Interstellar Boundary EXplorer

Plasma and magnetic fields in the heliosheath

This paper reviews recent results from the Voyager spacecraft in the heliosheath. The speed observed at Voyager 2 (V2) has been constant across the heliosheath, but the flow is turning significantly