The Importance of Using Continuous Solar Inputs in 3D Models to Simulate the Distant Solar Wind and Heliosheath

Details The Importance of Using Continuous Solar Inputs in 3D Models to Simulate the Distant Solar Wind and Heliosheath The Importance of Using Continuous Solar Inputs in 3D Models to Simulate the Distant Solar Wind and Heliosheath

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh14a1692i&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH14A-1692

Physics

2114 Energetic Particles (7514), 2126 Heliosphere/Interstellar Medium Interactions, 2139 Interplanetary Shocks, 2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2164 Solar Wind Plasma

Scientific paper

Solar transients and the background solar wind give rise to asymmetries in the distant solar wind and heliosheath. Entering continuous solar data into time-dependent, 3D models originating at the Sun is crucial for accurately characterizing the distant solar wind and the heliosheath. We employ our time-dependent, 3D MHD (magnetohydrodynamic) model the HHMS - the Hybrid Heliospheric Modeling System - to obtain insights into the propagation of the solar wind to ACE, Ulysses, and beyond. In addition, we use our quick look tool, the HAFv.2, a 3D, time-dependent kinematic model, to complement the HHMS results. Comparisons of simulations from both models with spacecraft data show very good agreement. We present case study results that contrast the significant differences between including and excluding specific features of models. These case studies illustrate that, in order to obtain a meaningful depiction of the heliosphere in 3D, it is necessary to use models that take primary solar source data as continuous inputs and extrapolate phenomena in three dimensions from the solar surface throughout the heliosphere and into the heliosheath. Models that are limited in their dimensionality (i.e., 1D or 2D), or limited temporally (i.e., non- continuous input data), or limited in terms of the starting or boundary conditions (e.g., starting at Earth), all lead to erroneous depictions of the time varying 3D heliosphere. For example, whereas the results from the 3D models with continuous inputs starting at the Sun agree with observations at Ulysses, even the results from the best 1D models differ considerably from the observations at Ulysses (e.g. the Halloween 2003 events). 3D modeling a solar event in isolation and not in the context of the continuous solar inputs leads to a very different longitudinal distribution of the event and its asymmetries (e.g., the January 2005 events). Modeling the heliospheric latitude variations in solar wind density starting with observations made at L1 rather than at the Sun leads to erroneous distributions (e.g. the Halloween 2003 events). Overall our results emphasize the significant asymmetries in three dimensions within the solar wind throughout the heliosphere. Moreover, these model and data comparisons provide the context for our studying solar transients and their effects on energetic particles, galactic cosmic rays, and turbulence in the distant solar wind and heliosheath.

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