What Can Global Models Combined with Observations Tell Us About the Structure of the Heliosphere? (Invited)

Details What Can Global Models Combined with Observations Tell Us About the Structure of the Heliosphere? (Invited) What Can Global Models Combined with Observations Tell Us About the Structure of the Heliosphere? (Invited)

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh24a..02p&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH24A-02

Physics

Plasma Physics

[2124] Interplanetary Physics / Heliopause And Solar Wind Termination, [2126] Interplanetary Physics / Heliosphere/Interstellar Medium Interactions, [7827] Space Plasma Physics / Kinetic And Mhd Theory

Scientific paper

While the Voyager 1 and 2 spacecraft are exploring the boundaries of the heliosphere, one of the newest NASA spacecraft, the Interstellar Boundary Explorer (IBEX) has started exploring the outermost reaches of the heliosphere measuring at 1 AU the fluxes of energetic neutral atoms (ENAs) created in the boundary regions separating the heliosphere from the LISM. The combination of in situ observations and three-dimensional, line-of-sight measurements gives us an opportunity that will not soon be repeated, i. e., to use numerical modeling to extract knowledge about the global heliospheric structure and solar wind (SW) and local interstellar medium (LISM) properties. A meaningful interpretation of spacecraft measurements is only possible if a numerical model uses observational boundary conditions and is properly validated against measurements themselves. This presentation reviews the current status of the modeling efforts and outlines the challenges facing the heliospheric community. The results presented include solar cycle calculations based on the Ulysses measurements accompanied by the WSO and NSO observations, the impact of the IBEX measurements on the development of numerical models, the comparison of time-dependent simulations with Voyager data in the supersonic SW and in the inner heliosheath, and SW calculations based on the remote photospheric observations. We also compare results obtained with numerical models of different level of complexity to identify physical processes that are essential for the proper interpretation of observational data.

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