Reconnection-driven Magnetohydrodynamic Turbulence in a Simulated Coronal-hole Jet

Uritsky, V. M.; Roberts, M. A.; DeVore, C. R.; Karpen, J. T.

doi:10.3847/1538-4357/aa5cb9

Cited by 27 publications

(29 citation statements)

References 61 publications

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“…Toward this end, many authors have investigated the connection between the plasma streams of increased bulk velocity and coronal jets (McComas et al 1995;Neugebauer et al 1995;Culhane et al 2007;Patsourakos et al 2008;Neugebauer 2012;Tian et al 2014) 2 . Since the Alfvénic fluctuations in the chromosphere contain a significant amount of energy (De Pontieu et al 2007), one possible interpretation of our in situ observations, also supported by extensive simulation work (Uritsky et al 2017;Wyper et al 2017;Roberts et al 2018), is that these fluctuations will continue to propagate even if a jet does not escape the Sun's gravity (Horbury et al 2020). Another candidate mechanism is interchange reconnection, which arises from magnetic flux transport close to the surface through structures such as coronal loops (van Ballegooijen et al 1998;Fisk & Schwadron 2001;Fisk 2005), interacting with open magnetic field lines to create S-shaped structure observed as a SB (Fisk & Kasper 2020;Zank et al 2020).…”

Section: A Mystery Of Switchback Originssupporting

confidence: 72%

Multiscale Solar Wind Turbulence Properties inside and near Switchbacks measured by Parker Solar Probe

Martinović,

Klein,

Huang

et al. 2021

Preprint

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Parker Solar Probe (PSP) routinely observes magnetic field deflections in the solar wind at distances less than 0.3 au from the Sun. These deflections are related to structures commonly called 'switchbacks' (SBs), whose origins and characteristic properties are currently debated. Here, we use a database of visually selected SB intervals-and regions of solar wind plasma measured just before and after each SB-to examine plasma parameters, turbulent spectra from inertial to dissipation scales, and intermittency effects in these intervals. We find that many features, such as perpendicular stochastic heating rates and turbulence spectral slopes are fairly similar inside and outside of SBs. However, important kinetic properties, such as the characteristic break scale between the inertial to dissipation ranges differ inside and outside these intervals, as does the level of intermittency, which is notably enhanced inside SBs and in their close proximity, most likely due to magnetic field and velocity shears observed at the edges. We conclude that the plasma inside and outside of a SB, in most of the observed cases, belongs to the same stream, and that the evolution of these structures is most likely regulated by kinetic processes, which dominate small scale structures at the SB edges.

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Section: A Mystery Of Switchback Originssupporting

confidence: 72%

Multiscale Solar Wind Turbulence Properties inside and near Switchbacks measured by Parker Solar Probe

Martinović,

Klein,

Huang

et al. 2021

Preprint

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“…Our idealized simulations' density fluctuation axial ratios are consistent with the lower end of the observed ranges and we are looking forward to investigating the propagation and evolution of these signatures into a solar wind outflow (e.g. Karpen et al 2017;Uritsky et al 2017). …”

Section: Reconnection-driven Solar Wind Outflow From Pseudostreamersmentioning

confidence: 93%

Formation and Reconnection of Three-dimensional Current Sheets with a Guide Field in the Solar Corona

Edmondson

Lynch

2017

ApJ

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We analyze a series of three-dimensional magnetohydrodynamic numerical simulations of magnetic reconnection in a model solar corona to study the effect of the guide field component on quasi-steady state interchange reconnection in a pseudostreamer arcade configuration. This work extends the analysis of Edmondson et al. (2010b) by quantifying the mass density enhancement coherency scale in the current sheet associated with magnetic island formation during the nonlinear phase of plasmoid-unstable reconnection. We compare the results of four simulations of a zero, weak, moderate, and a strong guide field, B GF /B 0 = {0.0, 0.1, 0.5, 1.0}, to quantify the plasmoid density enhancement's longitudinal and transverse coherency scales as a function of the guide field strength. We derive these coherency scales from autocorrelation and wavelet analyses, and demonstrate how these scales may be used to interpret the density en-

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“…One proposed mechanism for TAW creation at the Sun includes the reconnection associated with solar jets (Shibata & Uchida 1986). Explosive jet observations provide some of the most direct measurements of the Alfvénic propagation of magnetic field line twist into the solar corona and into the heliosphere (see Raouafi et al 2016;Uritsky et al 2017, and references therein). The highresolution simulations by Wyper et al (2016) resolved both the large-scale twist jet eruption along the external spine line and small-scale, 3D flux rope islands with localized, concentrated twist which were formed in the reconnection current sheet layer during the breakout/interchange reconnection prior to the main eruption (see also Lynch et al 2014;Wyper et al 2017).…”

Section: Torsional Alfvén Waves As "Pseudo-flux Rope" Structures Frommentioning

confidence: 99%

Structured Slow Solar Wind Variability: Streamer-blob Flux Ropes and Torsional Alfvén Waves

Higginson

Lynch

2018

ApJ

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The slow solar wind exhibits strong variability on timescales from minutes to days, likely related to magnetic reconnection processes in the extended solar corona. Higginson et al. (2017b) presented a numerical magnetohydrodynamic simulation which showed interchange magnetic reconnection is ubiquitous and most likely responsible for releasing much of the slow solar wind, in particular along topological features known as the Separatrix-Web (S-Web). Here, we continue our analysis, focusing on two specific aspects of structured slow solar wind variability. The first type is present in the slow solar wind found near the heliospheric current sheet, and the second we predict should be present everywhere S-Web slow solar wind is observed. For the first type, we examine the evolution of three-dimensional magnetic flux ropes formed at the top of the helmet streamer belt by reconnection in the heliospheric current sheet (HCS). For the second, we examine the simulated remote and in situ signatures of the large-scale torsional Alfvén wave (TAW) which propagates along an S-Web arc to high latitudes. We describe the similarities and differences between the reconnection-generated flux ropes in the HCS, which resemble the well-known "streamer blob" observations, and the similarly structured TAW. We discuss the implications of our results for the complexity of the HCS and surrounding plasma sheet, and the potential for particle acceleration, as well as the interchange reconnection scenarios which may generate TAWs in the solar corona. We discuss predictions from our simulation results for the dynamic slow solar wind in the extended corona and inner heliosphere.

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Reconnection-driven Magnetohydrodynamic Turbulence in a Simulated Coronal-hole Jet

Cited by 27 publications

References 61 publications

Multiscale Solar Wind Turbulence Properties inside and near Switchbacks measured by Parker Solar Probe

Multiscale Solar Wind Turbulence Properties inside and near Switchbacks measured by Parker Solar Probe

Formation and Reconnection of Three-dimensional Current Sheets with a Guide Field in the Solar Corona

Structured Slow Solar Wind Variability: Streamer-blob Flux Ropes and Torsional Alfvén Waves

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