Meridional motions and Reynolds stress from SDO/AIA coronal bright points data

Abstract

Context. It is possible to detect and track coronal bright points (CBPs) in SDO/AIA images. Combination of high resolution and high cadence provides a wealth of data that can be used to determine velocity flows on the solar surface with very high accuracy. Aims. We derived a very accurate solar rotation profile and investigated meridional flows, torsional oscillations and horizontal Reynolds stress based on $\approx$6 months of SDO/AIA data. Methods. We used a segmentation algorithm to detect CBPs in SDO/AIA images. We also used invariance of the solar rotation profile with central meridian distance (CMD) to determine the height of CBPs in 19.3 nm channel. Results. Best fit solar rotation profile is given by $\omega (b)=(14.4060\pm 0.0051+(-1.662\pm 0.050){\sin }^{2}b+(-2.742\pm 0.081){\sin }^{4}b)${\degr} day${}^{-1}$. Height of CBPs in SDO/AIA 19.3 nm channel was found to be $\approx$6500 km. Meridional motion is predominantly poleward for all latitudes, while solar velocity residuals show signs of torsional oscillations. Horizontal Reynolds stress was found to be small compared to similar works, but still showing transfer of angular momentum towards the solar equator. Conclusion. Most of the results are consistent with Doppler measurements rather than tracer measurements. Fairly small calculated value of horizontal Reynolds stress might be due to the particular phase of the solar cycle. Accuracy of the calculated rotation profile indicates that it is possible to measure changes in the profile as the solar cycle evolves. Analysis of further SDO/AIA CBP data will also help in better understanding of the temporal behaviour of the rotation velocity residuals, meridional motions and Reynolds stress.

References in corpus (4)

• Subsurface Meridional Circulation in the Active Belts
• Validity of the relations between the synodic and sidereal rotation velocities of the Sun
• Steps toward a high precision solar rotation profile: Results from SDO/AIA coronal bright point data
• Tracing sunspot groups to determine angular momentum transfer on the Sun

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• Differential rotation of the chromosphere in the He I absorption line
• Meridional Motions and Reynolds Stress Determined by Using Kanzelhöhe Drawings and White Light Solar Images from 1964 to 2016
• Differences in physical properties of coronal bright points and their ALMA counterparts within and outside coronal holes