DKIST Unveils the Serpentine Topology of Quiet Sun Magnetism in the Photosphere

Campbell, Ryan J.; Keys, P. H.; Mathioudakis, M.; Wöger, F.; Schad, T.; Tritschler, A.; de Wijn, A. G.; Smitha, H. N.; Beck, C.; Christian, D. J.; Jess, D. B.; Erdélyi, R.

doi:10.3847/2041-8213/acf85d

Cited by 6 publications

(1 citation statement)

References 66 publications

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“…This provides a wide range of scales over which reconnection begins in the fully coupled regime, so that neutrals are involved in the reconnection dynamics. These initial CSs have thicknesses a = 10-100 km, the upper end of the range being near the resolution limit of DKIST (Campbell et al 2023). Since this is also about the photon mean free path at the photosphere (Judge et al 2015), much thinner CSs would be visible only indirectly through their heating and brightening effects.…”

Section: Discussionmentioning

confidence: 95%

Applications of Fast Magnetic Reconnection Models to the Atmospheres of the Sun and Protoplanetary Disks

Pucci,

Singh,

Gorti

et al. 2024

ApJ

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Partially ionized plasmas consist of charged and neutral particles whose mutual collisions modify magnetic reconnection compared with the fully ionized case. The collisions alter the rate and locations of the magnetic dissipation heating and the distribution of energies among the particles accelerated into the nonthermal tail. We examine the collisional regimes for the onset of fast reconnection in two environments: the partially ionized layers of the solar atmosphere, and the protoplanetary disks that are the birthplaces for planets around young stars. In both these environments, magnetic nulls readily develop into resistive current sheets in the regime where the charged and neutral particles are fully coupled by collisions, but the current sheets quickly break down under the ideal tearing instability. The current sheets collapse repeatedly, forming magnetic islands at successively smaller scales, until they enter a collisionally decoupled regime where the magnetic energy is rapidly turned into heat and charged-particle kinetic energy. Small-scale, decoupled fast reconnection in the solar atmosphere may lead to preferential heating and energization of ions and electrons that escape into the corona. In protoplanetary disks such reconnection causes localized heating in the atmospheric layers that produce much of the infrared atomic and molecular line emission observed with the Spitzer and James Webb Space Telescopes.

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Section: Discussionmentioning

confidence: 95%

Applications of Fast Magnetic Reconnection Models to the Atmospheres of the Sun and Protoplanetary Disks

Pucci,

Singh,

Gorti

et al. 2024

ApJ

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Solar active region evolution and imminent flaring activity through color-coded visualization of photospheric vector magnetograms

Kontogiannis,

Pietrow,

Druett

et al. 2024

A&A

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The emergence of magnetic flux, its transition to complex configurations, and the pre-eruptive state of active regions are probed using photospheric magnetograms. Our aim is to pinpoint different evolutionary stages in emerging active regions, explore their differences, and produce parameters that could advance flare prediction using color-coded maps of the photospheric magnetic field. The three components of the photospheric magnetic field vector are combined to create color-combined magnetograms (COCOMAGs). From these, the areas occupied by different color hues are extracted, creating appropriate time series (color curves). These COCOMAGs and color curves are used as proxies of the active region evolution and its complexity. The morphology of COCOMAGs showcases typical features of active regions, such as sunspots, plages, and sheared polarity inversion lines. The color curves represent the area occupied by photospheric magnetic field of different orientation and contain information pertaining to the evolutionary stages of active regions. During emergence, most of the region area is dominated by horizontal or highly inclined magnetic field, which is gradually replaced by more vertical magnetic field. In complex regions, large parts are covered by highly inclined magnetic fields, appearing as abrupt color changes in COCOMAGs. The decay of a region is signified by a domination of vertical magnetic field, indicating a gradual relaxation of the magnetic field configuration. The color curves exhibit a varying degree of correlation with active region complexity. Particularly the red and magenta color curves, which represent strong, purely horizontal magnetic field, are good indicators of future flaring activity. Color-combined magnetograms facilitate a comprehensive view of the evolution of active regions and their complexity. They offer a framework for the treatment of complex observations and can be used in pattern recognition, feature extraction, and flare-prediction schemes.

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The US National Science Foundation Daniel K. Inouye Solar Telescope operations commissioning: results and lessons learned

Rimmele,

Tritschler,

Parraguez

et al. 2024

Ground-Based and Airborne Telescopes X

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DKIST Unveils the Serpentine Topology of Quiet Sun Magnetism in the Photosphere

Cited by 6 publications

References 66 publications

Applications of Fast Magnetic Reconnection Models to the Atmospheres of the Sun and Protoplanetary Disks

Applications of Fast Magnetic Reconnection Models to the Atmospheres of the Sun and Protoplanetary Disks

Solar active region evolution and imminent flaring activity through color-coded visualization of photospheric vector magnetograms

The US National Science Foundation Daniel K. Inouye Solar Telescope operations commissioning: results and lessons learned

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