The structure of magnetic turbulence in the heliosheath region observed by Voyager 2 at 106 AU

Kavli Affiliate: John D. Richardson

| First 5 Authors: Federico Fraternale, Nikolai V Pogorelov, John D Richardson, Daniela Tordella,

| Summary:

It is currently believed that the turbulent fluctuations pervade the
outermost heliosphere. Turbulence, magnetic reconnection, and their link may be
responsible for magnetic energy conversion in these regions. The governing
mechanisms of such anisotropic and compressible magnetic turbulence in the
inner heliosheath (IHS) and in the local interstellar medium (LISM) still lack
a thorough description. The present literature mainly concerns large scales
which are not representative of the inertial-cascade dynamics of turbulence.
Moreover, lack of broadband spectral analysis makes the IHS dynamics critically
understudied. Our recent study shows that 48 s magnetic-field data from the
Voyager mission are appropriate for a spectral analysis over a frequency range
of six decades, from 5 x 10-8 Hz to 10-2 Hz. Here, focusing on the Voyager 2
observation interval from 2013.824 to 2016.0, we describe the structure of
turbulence in a sector zone of the IHS. A spectral break around 7 x 10-7 Hz
(magnetic structures with size l~1.3 Astronomical Units) separates the
energy-injection regime from the inertial-cascade regime of turbulence. A
second scale is observed around 6 x 10-5 Hz (l~ 0.017 AU) and corresponds to a
peak of compressibility and intermittency of fluctuations.

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