A dynamic and realistic heliospheric modelling using interplanetary scintillation and photospheric magnetic data

Details A dynamic and realistic heliospheric modelling using interplanetary scintillation and photospheric magnetic data A dynamic and realistic heliospheric modelling using interplanetary scintillation and photospheric magnetic data

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh43d..04w&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH43D-04

Physics

[2126] Interplanetary Physics / Heliosphere/Interstellar Medium Interactions, [2134] Interplanetary Physics / Interplanetary Magnetic Fields, [2164] Interplanetary Physics / Solar Wind Plasma

Scientific paper

A new MHD simulation method for reproducing a realistic and time-varying global heliospheric modelling is developed using solar-wind speed data from interplanetary scintillation (IPS) of Nagoya University and photospheric magnetic data from the Wilcox Solar Observatory. These data sets provide inner boundary spherical surface conditions centered at 5 AU from the Sun and include both three-component solar-wind velocity and magnetic field. Hence it enables us to reproduce dynamical co-rotating wind-wind interactions and also magnetic field structures such as an oscillating equatorial magnetic neutral sheet in the three-dimensional heliosphere. In our results, a realistic and oscillating equatorial neutral sheet and periodic increases of temperature due to wind-wind interactions are reproduced during the period from December 6, 2000 to December 31, 2010, both in the interplanetary space and the heliosheath. The decrease of the mean solar wind density during the solar-cycle 23 from 5/cc to 3.5/cc at 1AU is taken into account. The interstellar magnetic field intensity is adopted as 4.6 micro G so that the observed V1-crossing with the termination shock is satisfied. The decrement degree of the solar-wind density around year 2006 is imposed to fit the observed V2-crossing with the termination shock. This simulation result is compared with that of previous simulation in which V2 plasma data were used as the inner boundary assuming an axisymmetric solar wind and a 3 micro G interstellar magnetic field intensity.

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