Multipoint Turbulence Analysis with HelioSwarm

Multipoint Turbulence Analysis with HelioSwarm Francesco Pecora http://orcid.org/0000-0003-4168-590X Sergio Servidio http://orcid.org/0000-0001-8184-2151 Leonardo Primavera http://orcid.org/0000-0001-7004-789X Antonella Greco http://orcid.org/0000-0001-5680-4487 Yan Yang http://orcid.org/0000-0003-2965-7906 William H. Matthaeus http://orcid.org/0000-0001-7224-6024 Abstract
Exploration of plasma dynamics in space, including turbulence, is entering a new era of multisatellite constellation measurements that will determine fundamental properties with unprecedented precision. Familiar but imprecise approximations will need to be abandoned and replaced with more-advanced approaches. We present a preparatory study of the evaluation of second- and third-order statistics, using simultaneous measurements at many points. Here, for specificity, the orbital configuration of the NASA Swarm mission is employed in conjunction with 3D magnetohydrodynamics numerical simulations of turbulence. The HelioSwarm nine-spacecraft constellation flies virtually through the turbulence to compare results with the exact numerical statistics. We demonstrate novel increment-based techniques for the computation of (1) the multidimensional spectra and (2) the turbulent energy flux. This latter increment-space estimate of the cascade rate, based on the third-order Yaglom–Politano–Pouquet theory, uses numerous increment-space tetrahedra. Our investigation reveals that HelioSwarm will provide crucial information on the nature of astrophysical turbulence.

Exploration of plasma dynamics in space, including turbulence, is entering a new era of multisatellite constellation measurements that will determine fundamental properties with unprecedented precision. Familiar but imprecise approximations will need to be abandoned and replaced with more-advanced approaches. We present a preparatory study of the evaluation of second- and third-order statistics, using simultaneous measurements at many points. Here, for specificity, the orbital configuration of the NASA Swarm mission is employed in conjunction with 3D magnetohydrodynamics numerical simulations of turbulence. The HelioSwarm nine-spacecraft constellation flies virtually through the turbulence to compare results with the exact numerical statistics. We demonstrate novel increment-based techniques for the computation of (1) the multidimensional spectra and (2) the turbulent energy flux. This latter increment-space estimate of the cascade rate, based on the third-order Yaglom–Politano–Pouquet theory, uses numerous increment-space tetrahedra. Our investigation reveals that HelioSwarm will provide crucial information on the nature of astrophysical turbulence.
03 08 2023 03 01 2023 L20 http://dx.doi.org/10.1088/crossmark-policy iopscience.iop.org Multipoint Turbulence Analysis with HelioSwarm The Astrophysical Journal Letters paper © 2023. The Author(s). Published by the American Astronomical Society. 2023-02-01 2023-02-08 2023-03-08 MMS Theory and Modeling 80NSSC19K0284 Parker Solar Probe Guest Investigator 80NSSC21K1765 PUNCH mission through SWRI N99054DS NSF-DOE AGS-2108834 EU Materia PONa3_00370 EC ∣ Horizon 2020 Framework Programme https://doi.org/10.13039/100010661 PON R&I 2014-20 http://creativecommons.org/licenses/by/4.0/ https://iopscience.iop.org/info/page/text-and-data-mining 10.3847/2041-8213/acbb03 https://iopscience.iop.org/article/10.3847/2041-8213/acbb03 https://iopscience.iop.org/article/10.3847/2041-8213/acbb03/pdf https://iopscience.iop.org/article/10.3847/2041-8213/acbb03/pdf https://iopscience.iop.org/article/10.3847/2041-8213/acbb03 https://iopscience.iop.org/article/10.3847/2041-8213/acbb03/pdf ApJ Bandyopadhyay 10.3847/1538-4357/aade04 866 106 2018 ApJS Bandyopadhyay 10.3847/1538-4365/ab5dae 246 48 2020 PhRvL Bandyopadhyay 10.1103/PhysRevLett.124.225101 124 2020 Batchelor 1953 Biskamp 10.1017/CBO9780511535222 2003 SSRv Burch 10.1007/s11214-015-0164-9 199 5 2016 JFM Comte-Bellot 10.1017/S0022112071001599 48 273 1971 SSRv Credland 10.1023/A:1004914822769 79 33 1997 JGRA Dunlop 10.1029/2001JA005088 107 1384 2002 Kepko 285 2018 PhR Marino 10.1016/j.physrep.2022.12.001 1006 1 2023 FrASS Maruca 10.3389/fspas.2021.665885 8 1 2021 JGR Matthaeus 10.1029/JA087iA08p06011 87 6011 1982 JAtS Orszag 10.1175/1520-0469(1971)028<1074:OTEOAI>2.0.CO;2 28 1074 1971 StAM Orszag 10.1002/sapm1972513253 51 253 1972 JFM Orszag 10.1017/S002211207900210X 90 129 1979 ApJL Osman 10.1086/510906 654 L103 2007 PhRvL Osman 10.1103/PhysRevLett.107.165001 107 2011 GeoRL Politano 10.1029/97GL03642 25 273 1998 EL Politano 10.1209/epl/i1998-00391-2 43 516 1998 Pope 10.1017/CBO9780511840531 2000 JFM Pouquet 10.1017/S0022112078001950 88 1 1978 ExA Retinò Online First 2021 PhRvL Servidio 10.1103/PhysRevLett.100.095005 100 2008 SoPh Sorriso-Valvo 10.1007/s11207-017-1229-6 293 10 2018 AGUFM Spence SH11B–04 2019 ApJ Verdini 10.1088/0004-637X/804/2/119 804 119 2015 ApJ Wang 10.3847/1538-4357/ac8f90 937 76 2022 PhPl Yamada 10.1063/1.2203950 13 2006