Data-driven Modeling of the Heliosphere

Details Data-driven Modeling of the Heliosphere Data-driven Modeling of the Heliosphere

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh43d..01p&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH43D-01

Physics

[2124] Interplanetary Physics / Heliopause And Solar Wind Termination, [2126] Interplanetary Physics / Heliosphere/Interstellar Medium Interactions, [2162] Interplanetary Physics / Solar Cycle Variations, [2164] Interplanetary Physics / Solar Wind Plasma

Scientific paper

Numerical model of the solar wind (SW) interaction with the local interstellar medium (LISM), developed in the UAHuntsville and implemented in the Multi-Scale Fluid-Kinetic Simulation Suite, treats ions magnetohydrodynamically while the transport of neutral atoms is performed kinetically by solving the Boltzmann equation with a Monte Carlo approach. Pickup ions (PUIs) can be treated as a separate fluid. The evolution of the PUI-generated turbulence is addressed on the differential level by adding three additional equations. Time-dependent, based on observational data, modeling of the SW in the entire heliosphere is critical for the interpretation of the IBEX and Voyager data. E. g., an unexpected decrease to negative values in the radial component of the SW velocity inferred from the Voyager 1 data is readily seen in our solar cycle simulations showing that unexpected sign of the SW velocity can extend as far as 10 AU inside the HP, while the regions of positive LISM radial velocities can extend up to 20 AU from the heliopause into the LISM. We use different sets of boundary conditions beyond the critical point to model time-dependent phenomena in the distant SW and in the heliosheath. In particular, we used Ulysses data to model the SW-LISM interaction during the period of the mission and match rather well the timing of the termination shock crossing by Voyager 1 and Voyager 2. Other sets of boundary conditions include those provided by the interplanetary scintillation measurements and obtained by numerical modeling of the inner heliosphere from the Sun's surface. Numerical results are extracted as time series along real spacecraft trajectories and compared with in situ measurements.

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