Solar Jets: SDO and IRIS Observations in the Perspective of New MHD Simulations

Schmieder, B.

doi:10.3389/fspas.2022.820183

Cited by 18 publications

(16 citation statements)

References 118 publications

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“…Because the value of the Ohmic resistivity coefficient in the solar corona is very small, this non-ideal effect is only relevant at very small scales, where it is possible to have very high values of current density concentrated in thin current sheets (Hornig & Priest 2003). Observations have shown bidirectional jets emerging from null points in the corona and photosphere (Schmieder et al 2022;Schmieder 2022), as well as in prominences (Hillier & Polito 2021), with velocities similar to the Alfvén speed, as is consistent with basic reconnection theory. The current sheets can become unstable, creating secondary magnetic structures often referred to as plasmoids (Shibata & Tanuma 2001).…”

Section: Introductionsupporting

confidence: 64%

Magnetic field amplification and structure formation by the Rayleigh-Taylor instability

Braileanu

Lukin

Khomenko

2023

A&A

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We report our results from a set of high-resolution, two-fluid, non-linear simulations of the magnetized Rayleigh Taylor instability (RTI) at the interface between a solar prominence and the corona. These data follow results reported earlier on linear and early non-linear RTI dynamics in this environment. This paper is focused on the generation and amplification of magnetic structures by RTI. The simulations use a two-fluid model that includes collisions between neutrals and charges, including ionization and recombination, energy and momentum transfer, and frictional heating. The 2.5D magnetized RTI simulations demonstrate that in a fully developed state of RTI, a large fraction of the gravitational energy of a prominence thread can be converted into quasi-turbulent energy of the magnetic field. The RTI magnetic energy generation is further accompanied by magnetic and plasma density structure formation, including dynamic formation, break-up, and merging of current sheets and plasmoid sub-structures. The flow decoupling between neutrals and charges, as well as ionization and recombination reactions, are shown to have significant impact on the structure formation in a magnetized RTI.

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Section: Introductionsupporting

confidence: 64%

Magnetic field amplification and structure formation by the Rayleigh-Taylor instability

Braileanu

Lukin

Khomenko

2023

A&A

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“…Numerical simulations recreate many of the aspects of this minifilament-eruption picture for producing jets (Wyper et al 2017(Wyper et al , 2018; those simulations emphasize the breakout reconnection (which we call the external reconnection above) in the formation of the jets, but the fundamental processes involved are as in the minifilament-eruption picture of Sterling et al (2015). Several reviews of coronal jets are available (e.g., Shimojo & Shibata 2000;Shibata & Magara 2011;Innes et al 2016;Raouafi et al 2016;Sterling 2018Sterling , 2021Hinode Review Team et al 2019;Shen 2021;Schmieder 2022).…”

Section: Introductionmentioning

confidence: 99%

Inconspicuous Solar Polar Coronal X-Ray Jets as the Source of Conspicuous Hinode/EUV Imaging Spectrometer Doppler Outflows

Sterling

Schwanitz

Harra

et al. 2022

ApJ

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We examine in greater detail five events previously identified as being sources of strong transient coronal outflows in a solar polar region in Hinode/Extreme Ultraviolet (EUV) Imaging Spectrometer (EIS) Doppler data. Although relatively compact or faint and inconspicuous in Hinode/X-ray Telescope (XRT) soft-X-ray (SXR) images and in Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) EUV images, we find that all of these events are consistent with being faint coronal X-ray jets. The evidence for this is that the events result from eruption of minifilaments of projected sizes spanning 5000–14,000 km and with erupting velocities spanning 19–46 km s−1, which are in the range of values observed in cases of confirmed X-ray polar coronal hole jets. In SXR images, and in some EUV images, all five events show base brightenings, and faint indications of a jet spire that (in four of five cases where determinable) moves away from the brightest base brightening; these properties are common to more obvious X-ray jets. For a comparatively low-latitude event, the minifilament erupts from near (≲few arcsec) a location of near-eruption-time opposite-polarity magnetic-flux-patch convergence, which again is consistent with many observed coronal jets. Thus, although too faint to be identified as jets a priori, otherwise all five events are identical to typical coronal jets. This suggests that jets may be more numerous than recognized in previous studies, and might contribute substantially to solar wind outflow, and to the population of magnetic switchbacks observed in Parker Solar Probe (PSP) data.

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“…Solar jets of all sizes are transient eruptive events. They appear as narrow structures that extend outward from the solar surface into the corona (Shibata & Magara 2011;Innes et al 2016;Raouafi et al 2016;Shen 2021;Schmieder 2022). They have often been observed in ultraviolet (UV; Pike & Mason 1998;Lu et al 2019;Zhang et al 2021a;Joshi et al 2021;Schmieder et al 2022), extreme ultraviolet (EUV; Wang et al 1998;Nisticò et al 2009;Schmieder et al 2013;Panesar et al 2016a;Sterling et al 2017), and X-ray images (Shibata et al 1992;Yokoyama & Shibata 1995;Alexander & Fletcher 1999;Moore et al 2018;Lee et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Genesis and Coronal-jet-generating Eruption of a Solar Minifilament Captured by IRIS Slit-raster Spectra

Panesar

Tiwari

Moore

et al. 2022

ApJ

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We present the first Mg ii slit-raster spectra from the Interface Region Imaging Spectrograph (IRIS) that fully capture the genesis and coronal-jet-generating eruption of a central-disk solar minifilament. The minifilament arose in a negative-magnetic-polarity coronal hole. The Mg ii spectroheliograms verify that the minifilament plasma temperature is chromospheric. The Mg ii spectra show that the erupting minifilament’s plasma has blueshifted upflow in the onset of the jet spire and simultaneous redshifted downflow at the location of the compact jet bright point (JBP). From the Mg ii spectra together with Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) EUV images and SDO/Helioseismic and Magnetic Imager (HMI) magnetograms, we find: (i) the minifilament forms above a flux-cancelation neutral line at an edge of a negative-polarity network flux clump; (ii) during the onset of the minifilament’s fast eruption and jet spire, the JBP begins brightening over the flux-cancelation neutral line. From IRIS2 inversion of the Mg ii spectra, the JBP’s Mg ii bright plasma has electron density, temperature, and downward (redshift) Doppler speed of 1012 cm−3, 6000 K, and 10 km s−1, respectively, and the growing spire shows clockwise spin. We speculate: (i) during the slow rise of the erupting minifilament-carrying a twisted flux rope, the top of the erupting flux-rope loop, by writhing, makes its field direction opposite to that of the encountered ambient far-reaching field; (ii) the erupting kink then can reconnect with the far-reaching field to create the spire and reconnect internally to create the JBP. We conclude that this coronal jet is normal in that magnetic flux cancelation builds a minifilament-carrying twisted flux rope and triggers the JBP-generating and jet-spire-generating eruption of the flux rope.

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Solar Jets: SDO and IRIS Observations in the Perspective of New MHD Simulations

Cited by 18 publications

References 118 publications

Magnetic field amplification and structure formation by the Rayleigh-Taylor instability

Magnetic field amplification and structure formation by the Rayleigh-Taylor instability

Inconspicuous Solar Polar Coronal X-Ray Jets as the Source of Conspicuous Hinode/EUV Imaging Spectrometer Doppler Outflows

Genesis and Coronal-jet-generating Eruption of a Solar Minifilament Captured by IRIS Slit-raster Spectra

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