Modeling Turbulence in the Distant Solar Wind

Details Modeling Turbulence in the Distant Solar Wind Modeling Turbulence in the Distant Solar Wind

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh11b1923k&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH11B-1923

Physics

[2149] Interplanetary Physics / Mhd Waves And Turbulence, [2152] Interplanetary Physics / Pickup Ions, [2164] Interplanetary Physics / Solar Wind Plasma

Scientific paper

Solar wind (SW) plasma consists of the thermal and nonthermal populations that interact with each other through wave-particle interaction due to turbulence generated by pickup ions (PUIs). This interaction substantially modifies the temperature of the core solar wind. PUIs are born when core SW ions experience charge exchange with the interstellar neutral atoms, which has also dynamical consequences for the distant SW because of its substantial deceleration. PUI pressure dominates in the vicinity of the heliospheric termination shock and therefore requires accurate modeling on the basis of theoretical prescriptions. We present a three-dimensional, time-dependent model of the turbulent SW in the presence of PUIs. Different turbulence models are compared seeking better agreement with in-situ measurements. Numerical simulations are performed in the region beyond the critical point and propagated to distances of 1-5 AU, where they are compared with the spacecraft data. Additionally, we use time-dependent boundary conditions from the ACE measurements to advance SW to the points on the Voyager trajectories where they are compared with observations.

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