Statistics – Computation
Scientific paper
May 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh23a..07o&link_type=abstract
American Geophysical Union, Spring Meeting 2005, abstract #SH23A-07
Statistics
Computation
2124 Heliopause And Solar Wind Termination, 2149 Mhd Waves And Turbulence, 2159 Plasma Waves And Turbulence, 7524 Magnetic Fields, 7827 Kinetic And Mhd Theory
Scientific paper
Effects of a Tilted Heliospheric Current Sheet in the Heliosheath Recent observations indicate that Voyager 1, now beyond 90 AU, is in a region unlike any encountered in it's 26 years of exploration. There is currently a controversy as to whether Voyager 1 has already crossed the Termination Shock, the first boundary of the Heliosphere (Krimigis et al. 2003; McDonald et al. 2003, Burlaga et al. 2003). An important aspect of this controversy is our poor understanding of this region. The region between the Termination Shock and the Heliopause, the Helisheath, is one of the most unknown regions theoretically. In the Heliosheath magnetic effects are crucial, as the solar magnetic field is compressed at the Termination Shock by the slowing flow. Therefore, to accurately model the heliosheath the inclusion of the solar magnetic field is crucial. Recently, our simulations showed that the Heliosheath presents remarkable dynamics, with turbulent flows and a presence of a jet flow at the current sheet that is unstable due to magnetohydrodynamic instabilities (Opher et al. 2003; 2004). We showed that to capture these phenomena, spatial numerical resolution is a crucial ingredient, therefore requiring the use of an adaptive mesh refinement (AMR). These previous works assumed that the solar rotation and the magnetic axis were aligned. Here we present including, for the first time, the tilt of the heliocurrent sheet using a 3D MHD AMR simulation with BATS-R-US code. We discuss the effects on the global structure of the Heliosheath, the flows, turbulence and magnetic field structure. We access the consequences for the observations measured by Voyager 1 since mid-2002. This intensive computational run was done at the supercomputer Columbia at NASA/AMES
Dezeeuw Darren
Gombosi Tamas
Liewer Paulett
Manchester Ward
Opher Merav
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