COSMIC RAY TRANSPORT IN HELIOSPHERIC MAGNETIC STRUCTURES. I. MODELING BACKGROUND SOLAR WIND USING THE CRONOS MAGNETOHYDRODYNAMIC CODE

Heliospheric evolution of solar wind small‐scale magnetic flux ropes

[1] We present results from the first comprehensive small‐scale flux rope survey between 0.3 and 5.5 AU using the Helios 1, Helios 2, IMP 8, Wind, ACE, and Ulysses spacecrafts to examine their occurrence rate, properties, and evolution. Small‐scale flux ropes are similar to magnetic clouds and can be modeled as a constant‐alpha, force‐free, cylindrically symmetric flux rope. They differ from ma...

Magnetohydrodynamic Modeling of Solar Magnetic Arcades Using Exponential Propagation Methods

Advanced numerical methods based on exponential propagation have been applied to mag netohydrodynamic MHD simulations This recently developed numerical technique e volves the system of nonlinear equations using exponential propagation of the Jacobian matrix The exponential of the matrix is approximated by projecting it onto the Krylov subspace using the Arnoldi algorithm The primary advantage o...

Understanding the Solar Wind-Mars Interaction with Global Magnetohydrodynamic Modeling

Small scale structures of the heliospheric magnetic field and the propagation of cosmic rays

___________________ Correspondence to: G. Erd V ([email protected]) Abstract. The heliospheric magnetic field is rich in highly fragmented small-scale structures. The magnetic background strongly influences the motion of the charged particles of relatively low rigidity. Using high time resolution magnetic field data measured by the magnetometer onboard Ulysses, we study the small-scale magneti...

The heliospheric modulation of cosmic ray protons during increased solar activity: effects of the position of the solar wind termination shock and of the heliopause

The effects on the modulation of cosmic ray protons of different positions for the solar wind termination shock and for the heliopause are illustrated for moderate solar maximum conditions. This is done with a numerical model which includes diffusive termination shock acceleration, a heliosheath and drifts. The modulation is computed for the heliospheric equatorial plane and at 35 heliolatitude...