Realistic and Time-Varying Outer Heliospheric Modeling by Three-Dimensional MHD Simulation

Details Realistic and Time-Varying Outer Heliospheric Modeling by Three-Dimensional MHD Simulation Realistic and Time-Varying Outer Heliospheric Modeling by Three-Dimensional MHD Simulation

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh24a..04w&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH24A-04

Physics

[2124] Interplanetary Physics / Heliopause And Solar Wind Termination, [2139] Interplanetary Physics / Interplanetary Shocks

Scientific paper

We aim at realistic and time-varying modeling which should satisfy both Voyager 1 (V1) and Voyager 2 (V2) observed crossing times of the termination shock (TS) simultaneously, by performing three-dimensional MHD simulations using a TVD scheme including the effects of neutral particles. Daily values of solar-wind speed and density observed by V2 are used at every simulation step so that short-term dynamical effects are reproduced. Before performing the dynamic simulation, we provide a 3D stationary solution using a set of standard parameters: the interstellar proton density is assumed to be 0.061/cc, neutral hydrogen density 0.176/cc, relative interstellar medium speed to the Sun 26.3 km/s and temperature 6300 Kelvin. Interstellar magnetic field intensity is 0.24nT and the orientation is oblique to the flow direction lying on the hydrogen deflection plane. The anisotropy of solar-wind speed is also taken into account so that the speed is 400 km/s in low latitudes and is 1.5 times higher in high latitudes. When the solar wind density at 1 AU is 5.1/cc and the latitudinal angle separating the high/low solar-wind speed regions is 30°, our dynamic simulations, which start from the above stationary solution, result in the targeting solution noted at the beginning. It is also clearly shown in these simulations that a) TS position increases every time when the solar-wind high-ram pressure pulse collides with the TS, b) a high magneto-sonic pulse is generated in the downstream side of the TS when the solar-wind high ram pressure pulse collides with the TS, c) fine structures of the heliosheath - magnetic wall and plasma sheet near the HP, and the thin current sheet embedded in the plasma sheet are identified, d) the magneto-sonic pulse is reflected at the plasma-sheet in the heliosheath, and the TS position decreases when the reflected pulse collides with the TS, and e) the time-varying radial distance between V2 and reproduced TS positions looks consistent with the TS particle intensity profile during the period when the TSP was observed at V2.

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