Evolution of Solar Wind Turbulence from 0.1 to 1 au during the First Parker Solar Probe–Solar Orbiter Radial Alignment

Telloni, Daniele; Sorriso‐Valvo, L.; Woodham, L. D.; Panasenco, O.; Velli, M.; Carbone, Francesco; Zank, G. P.; Bruno, R.; Perrone, D.; Nakanotani, M.; Shi, Chen; D’Amicis, R.; Marco, R. De; Jagarlamudi, V. K.; Steinvall, Konrad; Marino, Raffaele; Adhikari, L.; Zhao, Lingling; Liang, Haoming; Tenerani, Anna; Laker, R.; Horbury, T. S.; Bale, S. D.; Pulupa, M.; Malaspina, D.; MacDowall, R. J.; Goetz, K.; Wit, T. Dudok de; Harvey, P.; Kasper, J. C.; Korreck, K. E.; Larson, D. E.; Case, A. W.; Stevens, M. L.; Whittlesey, P. L.; Livi, R.; Owen, C. J.; Livi, S.; Louarn, P.; Antonucci, E.; Romoli, M.; O’Brien, H.; Evans, V.; Angelini, V.

doi:10.3847/2041-8213/abf7d1

Cited by 65 publications

(52 citation statements)

References 52 publications

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“…Particular attention has been paid to radial alignments between the two probes. Indeed, the first PSP-SO line-up occurred in 2020 September, allowing the radial evolution of solar wind turbulence between 0.1 and 1 au to be studied, i.e., from a highly Alfvénic and less developed turbulence state near the Sun to a fully developed and intermittent turbulence state close to the Earth (Telloni et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Exploring the Solar Wind from Its Source on the Corona into the Inner Heliosphere during the First Solar Orbiter–Parker Solar Probe Quadrature

Telloni

Andretta

Antonucci

et al. 2021

ApJL

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This Letter addresses the first Solar Orbiter (SO)-Parker Solar Probe (PSP) quadrature, occurring on 2021 January 18 to investigate the evolution of solar wind from the extended corona to the inner heliosphere. Assuming ballistic propagation, the same plasma volume observed remotely in the corona at altitudes between 3.5 and 6.3 solar radii above the solar limb with the Metis coronagraph on SO can be tracked to PSP, orbiting at 0.1 au, thus allowing the local properties of the solar wind to be linked to the coronal source region from where it originated. Thanks to the close approach of PSP to the Sun and the simultaneous Metis observation of the solar corona, the flow-aligned magnetic field and the bulk kinetic energy flux density can be empirically inferred along the coronal current sheet with an unprecedented accuracy, allowing in particular estimation of the Alfvén radius at 8.7 solar radii during the time of this event. This is thus the very first study of the same solar wind plasma as it expands from the sub-Alfvénic solar corona to just above the Alfvén surface.

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Section: Introductionmentioning

confidence: 99%

Exploring the Solar Wind from Its Source on the Corona into the Inner Heliosphere during the First Solar Orbiter–Parker Solar Probe Quadrature

Telloni

Andretta

Antonucci

et al. 2021

ApJL

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“…Tracing of the cross-helicity evolution with distance from the Sun provided one of the first clear lines of evidence that nonlinear dynamical evolution occurs in the solar wind . More recently (Telloni et al, 2021) measured a stream of solar wind at 0.1 and 1.0 AU and showed that the magnetic spectral density, flatness, and higher order moment scaling laws were consistent with Alfvénic fluctuations near the Sun evolving into fully developed turbulence. Similarly, (Chen et al, 2020) showed that turbulence evolves between 0.17 and 1 AU: at 0.17 AU the data showed increased energy spectral density, a slope of −3/2, lower magnetic compressibility, and increased relative amount of outward propagating Alfvénic fluctuations compared to inward.…”

Section: Turbulent Structuring In the Solar Windmentioning

confidence: 91%

Mesoscale Structure in the Solar Wind

Viall

DeForest

Kepko

2021

Front. Astron. Space Sci.

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Structures in the solar wind result from two basic mechanisms: structures injected or imposed directly by the Sun, and structures formed through processing en route as the solar wind advects outward and fills the heliosphere. On the largest scales, solar structures directly impose heliospheric structures, such as coronal holes imposing high speed streams of solar wind. Transient solar processes can inject large-scale structure directly into the heliosphere as well, such as coronal mass ejections. At the smallest, kinetic scales, the solar wind plasma continually evolves, converting energy into heat, and all structure at these scales is formed en route. “Mesoscale” structures, with scales at 1 AU in the approximate spatial range of 5–10,000 Mm and temporal range of 10 s–7 h, lie in the orders of magnitude gap between the two size-scale extremes. Structures of this size regime are created through both mechanisms. Competition between the imposed and injected structures with turbulent and other evolution leads to complex structuring and dynamics. The goal is to understand this interplay and to determine which type of mesoscale structures dominate the solar wind under which conditions. However, the mesoscale regime is also the region of observation space that is grossly under-sampled. The sparse in situ measurements that currently exist are only able to measure individual instances of discrete structures, and are not capable of following their evolution or spatial extent. Remote imaging has captured global and large scale features and their evolution, but does not yet have the sensitivity to measure most mesoscale structures and their evolution. Similarly, simulations cannot model the global system while simultaneously resolving kinetic effects. It is important to understand the source and evolution of solar wind mesoscale structures because they contain information on how the Sun forms the solar wind, and constrains the physics of turbulent processes. Mesoscale structures also comprise the ground state of space weather, continually buffeting planetary magnetospheres. In this paper we describe the current understanding of the formation and evolution mechanisms of mesoscale structures in the solar wind, their characteristics, implications, and future steps for research progress on this topic.

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“…This has allowed models of solar wind to be constrained by measurements at different radial distances to the Sun. In particular, the characteristics of MHD turbulence in solar wind are continuously being investigated (e.g., [145][146][147][148][149]), and very recent results show signatures of wave-driven turbulence extending much closer to the Sun [9,[150][151][152].…”

Section: Propagating Wavesmentioning

confidence: 99%

How Transverse Waves Drive Turbulence in the Solar Corona

Howson

2022

Symmetry

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Oscillatory power is pervasive throughout the solar corona, and magnetohydrodynamic (MHD) waves may carry a significant energy flux throughout the Sun’s atmosphere. As a result, over much of the past century, these waves have attracted great interest in the context of the coronal heating problem. They are a potential source of the energy required to maintain the high-temperature plasma and may accelerate the fast solar wind. Despite many observations of coronal waves, large uncertainties inhibit reliable estimates of their exact energy flux, and as such, it remains unclear whether they can contribute significantly to the coronal energy budget. A related issue concerns whether the wave energy can be dissipated over sufficiently short time scales to balance the atmospheric losses. For typical coronal parameters, energy dissipation rates are very low and, thus, any heating model must efficiently generate very small-length scales. As such, MHD turbulence is a promising plasma phenomenon for dissipating large quantities of energy quickly and over a large volume. In recent years, with advances in computational and observational power, much research has highlighted how MHD waves can drive complex turbulent behaviour in the solar corona. In this review, we present recent results that illuminate the energetics of these oscillatory processes and discuss how transverse waves may cause instability and turbulence in the Sun’s atmosphere.

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Evolution of Solar Wind Turbulence from 0.1 to 1 au during the First Parker Solar Probe–Solar Orbiter Radial Alignment

Cited by 65 publications

References 52 publications

Exploring the Solar Wind from Its Source on the Corona into the Inner Heliosphere during the First Solar Orbiter–Parker Solar Probe Quadrature

Exploring the Solar Wind from Its Source on the Corona into the Inner Heliosphere during the First Solar Orbiter–Parker Solar Probe Quadrature

Mesoscale Structure in the Solar Wind

How Transverse Waves Drive Turbulence in the Solar Corona

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