Tracked Motions of G-band Bright Points

Details Tracked Motions of G-band Bright Points Tracked Motions of G-band Bright Points

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21715503t&link_type=abstract

American Astronomical Society, AAS Meeting #217, #155.03; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Scientific paper

Abstract
Bright points (BPs) are magnetic elements in the photosphere observable in the CN G-band at 4305 Å. High-speed speckle images were taken with the Dunn Solar Telescope in Sunspot, NM with a 80 frame burst every 32 seconds, achieving a resolution of 0.1422” in the reconstructed images. The BPs were tracked by hand and velocities and curls (vorticity) were derived at each time step. Small-scale motions were also tracked using a FFT local correlation tracking algorithm. The velocities obtained from correlation tracking were generally smaller by factors of 2 to 5 than the hand tracked motion in agreement with previous results, however, the hand-tracked BPs tended to move in the direction of the local correlation tracking velocities. The velocities of the BPs were used to estimate the energy associated with these motions, which was found to vary between 1 to 3*1017 erg cm-1 based on observed velocities between 2 to 7 km s-1. This amount of energy could provide a source of heat for the corona, which has a minimum energy requirement of 106 erg cm-2 s-1. In some cases, BPs were seen to travel at 7 km s-1, and changed their direction of motion after collisions with granules. These supersonic speeds could generate shockwaves, which in turn could transfer energy from the BPs to the magnetic field. BPs often spiral around each other, possibly entangling the associated magnetic field providing a mechanism by which energy could be transported to the corona.
This research was funded by the National Science Foundation as part of its REU program.

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