Solar Cycle Model Based on Ulysses Measurements (Invited)

Details Solar Cycle Model Based on Ulysses Measurements (Invited) Solar Cycle Model Based on Ulysses Measurements (Invited)

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh24a..02p&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH24A-02

Physics

Plasma Physics

[7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7536] Solar Physics, Astrophysics, And Astronomy / Solar Activity Cycle, [7837] Space Plasma Physics / Neutral Particles

Scientific paper

The outer heliosphere is formed due to the interaction of the solar wind (SW) with the local interstellar medium (LISM). Heliospheric models have matured enough to allow us a quantitative comparison of the simulation results with the measurements performed by a fleet of spacecraft cruising the SW at distances starting at 1 AU out into the heliosheath. Solar cycle effects are of fundamental importance for understanding the structure of the heliosphere. This is because of highly dynamic variations of the SW parameters, in particular, in the latitudinal extent of the slow SW and the tilt between the Sun’s magnetic and rotation axes. The Ulysses spacecraft provided us a unique set of observational data measured during its pole-to-pole flybys. These revealed a substantial decrease of the SW ram pressure during the 3rd pole-to-pole orbit as compared to the 1st. Both orbits measured SW properties in the vicinity of the corresponding solar activity minima. We use Ulysses and Wilcox Solar Observatory data to create a time-dependent, three-dimensional model of the solar cycle. The first results obtained with this model reveal new features in the plasma and magnetic field distributions and may be of importance for the interpretation of Voyager observations in the inner heliosheath.

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