Modeling the Outer Heliosphere with Realistic, Time-dependent Boundary Conditions in the Solar Wind

Details Modeling the Outer Heliosphere with Realistic, Time-dependent Boundary Conditions in the Solar Wind Modeling the Outer Heliosphere with Realistic, Time-dependent Boundary Conditions in the Solar Wind

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh31c..04p&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SH31C-04

Astronomy and Astrophysics

Astronomy

2102 Corotating Streams, 2124 Heliopause And Solar Wind Termination, 7536 Solar Activity Cycle (2162), 7537 Solar And Stellar Variability (1650)

Scientific paper

Interaction of the solar wind (SW) with the local interstellar medium (LISM) creates an outer heliosphere whose properties are substantially influenced by charge exchange between charged and neutral particles in a partially ionized plasma. The characteristic size of the heliosphere, including the tail region, is a few thousand astronomical units (AU). The heliospheric termination shock (TS) was crossed by the Voyager 1 and Voyager 2 spacecraft approximately at 94 and 84 AU, respectively. If we assume that the angle between the Sun's rotation and magnetic axes is constant, for a spherically symmetric SW, the distance between two consecutive locations of the heliospheric current sheet (HCS) along a SW streamline belonging to the ecliptic plane is about 3 AU. This difference in length scales creates a challenge for modeling the propagation of realistic, time-dependent SW to the TS and further into the inner heliosheath. Moreover, the LISM plasma is affected by perturbations in the shape of the heliopause. The propagation of a global merged interaction region (GMIR) into the outer heliosheath is thought to generate 2-3 kHz radio emission. In this presentation, we investigate the effect of the solar cycle on the SW-LISM interaction. We also analyze the effect of a GMIR on the conditions ensuring radio emission. An attempt is made to use time-dependent SW and interplanetary magnetic field parameters obtained at 5-10 AU from the numerical model of the inner heliosphere as boundary conditions for analyzing time-dependent properties of the outer heliosphere.

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