Insights gained using HHMS-PI from the Sun to Voyager 2

We extended the three-dimensional (3D) time-dependent magnetohydrodynamic (MHD) Hybrid Heliospheric Modeling System with Pickup Protons (HHMS-PI) [1] out to Voyager 2 (V2) and to 75 AU. HHMS-PI starts at the Sun and uses pre-and post-event background mode source surface (SS) solar inputs and solar event inputs. Our scientific results include good agreement between the HHMS-PI simulated parameters of the solar wind (SW) and interplanetary magnetic field (IMF) measurements at ACE, Ulysses, and Cassini. HHMS-PI simulates well the strong shocks observed at ACE, Ulysses, and Cassini associated with the Halloween 2003 solar events. This agreement indicates that HHMS-PI can provide good simulations for the Sedov strong shock limit. Comparisons between HHMS-PI simulated shock propagation from the Sun to Ulysses and Cassini and the spacecraft measurements of shock arrivals indicates that pickup protons slow the propagation of shocks to Ulysses and Cassini. Our simulations also demonstrate the importance of asymmetric flows in latitude and in longitude. For the Halloween 2003 solar events the HHMS-PI simulations show the large extent in latitude and in longitude of the shocks. The HHMS-PI simulations also indicate that IMF sector boundaries are greatly affected by the SW/IMF.