Inner-Heliosphere Signatures of Ion-Scale Dissipation and Nonlinear Interaction. (arXiv:2001.05081v1 [astro-ph.SR])

Inner-Heliosphere Signatures of Ion-Scale Dissipation and Nonlinear Interaction. (arXiv:2001.05081v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bowen_T/0/1/0/all/0/1">Trevor A. Bowen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mallet_A/0/1/0/all/0/1">Alfred Mallet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bale_S/0/1/0/all/0/1">Stuart D. Bale</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonnell_J/0/1/0/all/0/1">J. W. Bonnell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Case_A/0/1/0/all/0/1">Anthony W. Case</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chandran_B/0/1/0/all/0/1">Benjamin D. G. Chandran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chasapis_A/0/1/0/all/0/1">Alexandros Chasapis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_C/0/1/0/all/0/1">Christopher H. K. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duan_D/0/1/0/all/0/1">Die Duan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wit_T/0/1/0/all/0/1">Thierry Dudok de Wit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goetz_K/0/1/0/all/0/1">Keith Goetz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Halekas_J/0/1/0/all/0/1">Jasper Halekas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harvey_P/0/1/0/all/0/1">Peter R. Harvey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kasper_J/0/1/0/all/0/1">J. C. Kasper</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Korreck_K/0/1/0/all/0/1">Kelly E. Korreck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Larson_D/0/1/0/all/0/1">Davin Larson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Livi_R/0/1/0/all/0/1">Roberto Livi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+MacDowall_R/0/1/0/all/0/1">Robert J. MacDowall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malaspina_D/0/1/0/all/0/1">David M. Malaspina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pulupa_M/0/1/0/all/0/1">Marc Pulupa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stevens_M/0/1/0/all/0/1">Michael Stevens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Whittlesey_P/0/1/0/all/0/1">Phyllis Whittlesey</a>

We perform a statistical study of the turbulent power spectrum at inertial
and kinetic scales observed during the first perihelion encounter of Parker
Solar Probe. We find that often there is an extremely steep scaling range of
the power spectrum just above the ion-kinetic scales, similar to prior
observations at 1 AU, with a power-law index of around $-4$. Based on our
measurements, we demonstrate that either a significant ($>50%$) fraction of
the total turbulent energy flux is dissipated in this range of scales, or the
characteristic nonlinear interaction time of the turbulence decreases
dramatically from the expectation based solely on the dispersive nature of
nonlinearly interacting kinetic Alfv’en waves.

We perform a statistical study of the turbulent power spectrum at inertial
and kinetic scales observed during the first perihelion encounter of Parker
Solar Probe. We find that often there is an extremely steep scaling range of
the power spectrum just above the ion-kinetic scales, similar to prior
observations at 1 AU, with a power-law index of around $-4$. Based on our
measurements, we demonstrate that either a significant ($>50%$) fraction of
the total turbulent energy flux is dissipated in this range of scales, or the
characteristic nonlinear interaction time of the turbulence decreases
dramatically from the expectation based solely on the dispersive nature of
nonlinearly interacting kinetic Alfv’en waves.

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