SH016-0014
Solar Wind Turbulence from 1 to 45 AU

Wednesday, 9 December 2020
Poster
Zackary Bradley Pine1, Charles William Smith2, Sophia Hollick3, Matthew R Argall2, Bernard John Vasquez2, Philip A Isenberg4, Nathan Schwadron2, Colin Joyce5, Justyna M Sokol6, Maciej Bzowski7, Megan L. McLaurin8, Kathleen E Hamilton9 and Robert James Leamon10, (1)Boston University, Boston, MA, United States, (2)University of New Hampshire, Durham, NH, United States, (3)Providence, RI, United States, (4)Univ New Hampshire, Durham, NH, United States, (5)Princeton University, Department of Astrophysical Sciences, Princeton, NJ, United States, (6)Space Research Center Polish Academy of Sciences, Warszawa, Poland, (7)Space Research Centre Polish Academy of Sciences, Warsaw, Poland, (8)Wolters Kluwer, Waltham, MA, United States, (9)Oak Ridge National Laboratory, Quantum Computing Institute, Oak Ridge, TN, United States, (10)NASA Headquarters, Washington, DC, United States
Abstract:
We review five recent publications that extend magnetic turbulence studies that were
pioneered using data from 1 AU to now include Voyager observations from 1977 through 1990
and 1 to 45 AU. We examine the spectral scale at which evidence of dissipation sets in and
evaluate the spectral indices, anisotropies, polarizations, and spectral transfer of energy. We
compare the latter to predictions from transport theory and the rate of energy injection
through wave excitation by newborn interstellar pickup ions. While many of our results agree
with conclusions from 1 AU, we find that the magnetic spectral anisotropy that relates to the
underlying anisotropy of the wave vectors exceeds theoretical predications for reasons we are
unable to determine. We also establish that wave energy excitation by newborn interstellar
pickup H+ forms the dominant energy source driving the turbulence beyond 10 AU.
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