Association of Calcium Network Bright Points with Underneath Photospheric Magnetic Patches

Narang, Nancy; Banerjee, D.; Chandrashekhar, K.; Pant, Vaibhav

doi:10.1007/s11207-019-1419-5

Cited by 3 publications

(2 citation statements)

References 26 publications

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“…Bright points usually correspond with kilogauss concentrations of vertical magnetic flux (Utz et al 2013), sometimes called flux elements, which are believed to be the bases of flux tubes that may rise to the corona, making them the source of much of the open magnetic flux in coronal holes (Hofmeister et al 2019). The rise of these flux tubes to the low chromosphere has been observed as brightenings in the chromospheric line Ca II H coinciding with photospheric bright points (Xiong et al 2017;Liu et al 2018b;Narang et al 2019). As they rise, these flux tubes expand rapidly (Kuckein 2019) due to the decreasing plasma pressure (Spruit 1976).…”

Section: Introductionmentioning

confidence: 99%

Characterizing the Motion of Solar Magnetic Bright Points at High Resolution

Kooten

Cranmer

2017

ApJ

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Magnetic bright points in the solar photosphere, visible in both continuum and G-band images, indicate footpoints of kilogauss magnetic flux tubes extending to the corona. The power spectrum of bright-point motion is thus also the power spectrum of Alfvén wave excitation, transporting energy up flux tubes into the corona. This spectrum is a key input in coronal and heliospheric models. We produce a power spectrum of bright-point motion using radiative magnetohydrodynamic simulations, exploiting spatial resolution higher than can be obtained in present-day observations, while using automated tracking to produce large data quantities. We find slightly higher amounts of power at all frequencies compared to observation-based spectra, while confirming the spectrum shape of recent observations. This also provides a prediction for observations of bright points with DKIST, which will achieve similar resolution and high sensitivity. We also find a granule size distribution in support of an observed twopopulation distribution, and we present results from tracking passive tracers which show a similar power spectrum to that of bright points. Finally, we introduce a simplified, laminar model of granulation, with which we explore the roles of turbulence and of the properties of the granulation pattern in determining bright-point motion.From these MURaM simulations, we extracted granule size distributions, the motion paths of passive tracers, and the motion paths of automatically-identified bright points. This

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Section: Introductionmentioning

confidence: 99%

Characterizing the Motion of Solar Magnetic Bright Points at High Resolution

Kooten

Cranmer

2017

ApJ

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Section: Introductionmentioning

confidence: 99%

Using Bright Point Shapes to Constrain Wave Heating of the Solar Corona: Predictions for DKIST

Van Kooten,

Cranmer

2024

ApJ

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Magnetic bright points on the solar photosphere mark the footpoints of kilogauss magnetic flux tubes extending toward the corona. Convective buffeting of these tubes is believed to excite magnetohydrodynamic waves, which can propagate to the corona and deposit heat there. Measuring wave excitation via bright point motion can thus constrain coronal and heliospheric models, and this has been done extensively with centroid tracking, which can estimate kink-mode wave excitation. DKIST is the first telescope to provide well-resolved observations of bright points, allowing shape and size measurements to probe the excitation of other wave modes that have been difficult, if not impossible, to study to date. In this work, we demonstrate a method of automatic bright point tracking that robustly identifies the shapes of bright points, and we develop a technique for interpreting measured bright point shape changes as the driving of a range of thin-tube wave modes. We demonstrate these techniques on a MURaM simulation of DKIST-like resolution. These initial results suggest that modes other than the long-studied kink mode could increase the total available energy budget for wave heating by 50%. Pending observational verification as well as modeling of the propagation and dissipation of these additional wave modes, this could represent a significant increase in the potency of wave-turbulence heating models.

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