Plasma Upflows Induced by Magnetic Reconnection Above an Eruptive Flux Rope

Baker, D.; Mihailescu, Teodora; Démoulin, P.; Green, Lucie M.; Driel-Gesztelyi, L. van; Valori, G.; Brooks, David H.; Long, David M.; Janvier, Miho

doi:10.1007/s11207-021-01849-7

Cited by 4 publications

(3 citation statements)

References 47 publications

(88 reference statements)

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“…In addition, Mandrini et al (2015) reported that AR plasma upflows observed by EIS and QSLs located by analyzing extrapolated field lines were found to evolve in parallel, both temporarily and spatially. Baker et al (2017Baker et al ( , 2021 had carried out similar analysis and interpretation of the driver of plasma upflows in ARs. Hence, it has been inferred that strong and dominant QSLs (with or without magnetic nulls) are the preferential positions for accumulation of strong current and the occurrence of magnetic reconnection resulting in observed plasma outflows in solar ARs.…”

Section: Discussionmentioning

confidence: 99%

Reconnection-generated Plasma Flows in the Quasi-separatrix Layer in Localized Solar Corona

Sripan

Srivastava

Mishra

et al. 2023

ApJ

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Multiwavelength observations of the propagating disturbances (PDs), discovered by Atmospheric Imaging Assembly (AIA) on board Solar Dynamics Observatory (SDO), are analyzed to determine their driving mechanism and physical nature. Two magnetic strands in the localized corona are observed to approach and merge with each other, followed by the generation of brightening, which further propagates in a cusp-shaped magnetic channel. Differential emission measure analysis shows an occurrence of heating in this region of interest. We extrapolate potential magnetic field lines at coronal heights from the observed Helioseismic and Magnetic Imager vector magnetogram via Green’s function method using MPI-AMRVAC. We analyze the field to locate magnetic nulls and quasi-separatrix layers (QSLs), which are preferential locations for magnetic reconnection. Dominant QSLs including a magnetic null are found to exist and match the geometry followed by PDs; therefore, this provides conclusive evidence of magnetic reconnection. In addition, spectroscopic analysis of Interface Region Imaging Spectrograph Si iv λ1393.77 line profiles show a rise of line width in the same time range depicting the presence of mass motion in the observed cusp-shaped region. PDs are observed to exhibit periodicities of around 4 minutes. The speeds of PDs measured by the surfing transform technique are close to each other in four different SDO/AIA bandpasses, i.e., 304, 171, 193, and 131 Å, excluding the interpretation of PDs in terms of slow magnetoacoustic waves. We describe comprehensively the observed PDs as quasiperiodic plasma flows generated as a result of periodic reconnection in the vicinity of a coronal magnetic null.

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Section: Discussionmentioning

confidence: 99%

Reconnection-generated Plasma Flows in the Quasi-separatrix Layer in Localized Solar Corona

Sripan

Srivastava

Mishra

et al. 2023

ApJ

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“…This enhancement suggests that there are at least two components of unresolved plasma upflow along the LOS (Tian et al 2021); namely, the background plasma flow (primary component) and high-speed upflow (secondary component). The strong secondary components have previously been observed in the upflows from active region boundaries (e.g., Yardley et al 2021a;Baker et al 2021) and coronal dimming (Tian et al 2012;Veronig et al 2019). They can be identified by fitting a double Gaussian instead of a single Gaussian function to the profile.…”

Section: Spatially Averaged Pixel Analysismentioning

confidence: 99%

The Merging of a Coronal Dimming and the Southern Polar Coronal Hole

Ngampoopun

Long

Baker

et al. 2023

ApJ

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We report on the merging between the southern polar coronal hole and an adjacent coronal dimming induced by a coronal mass ejection on 2022 March 18, resulting in the merged region persisting for at least 72 hr. We use remote sensing data from multiple co-observing spacecraft to understand the physical processes during this merging event. The evolution of the merger is examined using Extreme-UltraViolet (EUV) images obtained from the Atmospheric Imaging Assembly on board the Solar Dynamic Observatory and Extreme Ultraviolet Imager, which is on board the Solar Orbiter spacecraft. The plasma dynamics are quantified using spectroscopic data obtained from the EUV Imaging Spectrometer on board Hinode. The photospheric magnetograms from the Helioseismic and Magnetic Imager are used to derive the magnetic field properties. To our knowledge, this work is the first spectroscopical analysis of the merging of two open-field structures. We find that the coronal hole and the coronal dimming become indistinguishable after the merging. The upflow speeds inside the coronal dimming become more similar to that of a coronal hole, with a mixture of plasma upflows and downflows observable after the merging. The brightening of the bright points and the appearance of coronal jets inside the merged region further imply ongoing reconnection processes. We propose that component reconnection between the coronal hole and coronal dimming fields plays an important role during this merging event because the footpoint switching resulting from the reconnection allows the coronal dimming to intrude onto the boundary of the southern polar coronal hole.

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“…To understand the topology of the magnetic field (e.g. van Driel-Gesztelyi et al 2012;Boe et al 2020;Baker et al 2021) and how stellar wind flows through a corona (e.g. Neugebauer et al 1998;Stansby et al 2020a), magnetic field line connectivities between the outer and inner boundaries are also needed, which requires tracing magnetic field lines through the threedimensional magnetic field solution using a field line tracer.…”

Section: Introductionmentioning

confidence: 99%

Test Problems for Potential Field Source Surface Extrapolations of Solar and Stellar Magnetic Fields

Stansby¹,

Verscharen²

2022

Preprint

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The potential field source surface (PFSS) equations are commonly used to model the coronal magnetic field of the Sun and other stars. As with any computational model, solving equations using a numerical scheme introduces errors due to discretisation. We present a set of tests for quantifying these errors by taking advantage of analytic solutions to the PFSS equations when the input field is proportional to a single spherical harmonic. From the spherical harmonic solutions we derive analytic equations for magnetic field lines traced through the three dimensional magnetic field solution. We propose these as a set of standard analytic solutions that all PFSS solvers should be tested against to quantify their inherent errors. We apply these tests to the pfsspy software package, showing that it reproduces spherical harmonic solutions well with a slight overestimation of the unsigned open magnetic flux. It is also successful at reproducing analytic field line equations, with errors in field line footpoints typically much less than one degree.

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Plasma Upflows Induced by Magnetic Reconnection Above an Eruptive Flux Rope

Cited by 4 publications

References 47 publications

Reconnection-generated Plasma Flows in the Quasi-separatrix Layer in Localized Solar Corona

Reconnection-generated Plasma Flows in the Quasi-separatrix Layer in Localized Solar Corona

The Merging of a Coronal Dimming and the Southern Polar Coronal Hole

Test Problems for Potential Field Source Surface Extrapolations of Solar and Stellar Magnetic Fields

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