Computer Science – Sound
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agusmsh51a..07w&link_type=abstract
American Geophysical Union, Spring Meeting 2007, abstract #SH51A-07
Computer Science
Sound
0545 Modeling (4255), 2104 Cosmic Rays, 2124 Heliopause And Solar Wind Termination, 2126 Heliosphere/Interstellar Medium Interactions, 2149 Mhd Waves And Turbulence (2752, 6050, 7836)
Scientific paper
The fact that Voyager 1 crossed the termination shock (TS) at 94 AU at the end of the year 2004 possibly provides us with some information on pressure conditions of the LISM, as well as the time-varying distance of the TS before and after the crossing. Our three-dimensional MHD simulation aims to reproduce the real dynamical heliosphere of the recent period, Sept. 10, 2001-Dec. 3, 2006. The Voyager 2 (V2) solar-wind data were used as the inner-boundary condition of the simulation. Initially the total pressure of the LISM is roughly defined so that V1 crossed the TS at 94 AU. The relation between the solar-wind ram-pressure and the time-varying TS motion is investigated. The TS is found to move almost parallel to V1, and was always very near V1 during the period from about September 2002, when the TS-particles were first observed at V1, to the time of the TS-crossing. At the end of the high ram-pressure pulses of the Halloween events around August, 2004, the TS began to move inward and then V1 crossed the TS. This TS inward motion continued for 1.2 years and the final TS location was at about 85 AU from the sun. Then the TS started to move outward again, and it reached about 95 AU by the end of our simulation. The motion of the Heliopause (HP) is found to move synchronously with the TS motion with a time- delay of 0.82 year. This time is roughly equal to the propagation time of the sound wave between the TS and the HP along the sun-V1 line. The relation between the TS-particle events and the motion of the TS-position is also considered. The motion of the TS is found to be well synchronized to the observed count of the TS-particles. Structures of the TS along the sun-V1 line are also studied in detail to relate to the TS-particles observations more clearly. The observation that the TS-particle count did not increase but rather decreased at the TS-crossing can be explained if the high ram-pressure pulse carries accelerated-particles toward the downstream side when it collides the TS. We also discuss the solar-wind deceleration between the positions of V1 and V2 by estimating the time-correlation between the simulated-magnetic-field at the V1 position with the observed V1 magnetic field. Our analysis indicates that the time delay due to the deceleration is about 15 days in the course of about 80 days journey of the solar wind for about 20 AU between positions of V2 and V1. The motion of the TS along the sun-V2 line is also discussed.
Hu Qiang
Tanaka Toshiaki
Washimi Haruichi
Zank Gary P.
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