NASA SDO - Interactions, Dec 9-10, 2012

A key to understanding the dynamics of the Sun and what causes the great solar explosions there relies on deciphering how material, heat and energy swirl across the Sun's surface and rise into the upper atmosphere, or corona. Tracking the constantly moving material requires state-of-the-art telescopes with the highest resolution possible.

Observing coronal loops, which are giant arcs of solar material constrained to travel along that particular path by the magnetic fields in the sun's atmosphere, help scientists learn more about the workings of the Sun. These loops can vary in complexity over the Sun's 11-year activity cycle, becoming more or less intertwined and inter-connected. Observations of this phenomena can help researchers understand what's happening with our star's complicated magnetic fields that can also power great eruptions on the Sun such as the solar flares or coronal mass ejections.

This segment captures approx. 38 hours from December 9 to 10, 2012 and shows the 171 angstroms wavelength. This channel is particularly good for observing coronal loops. This area shows the Active Region 1629 and 1630 and their interactions with each other. Also visible is a nice flow along a filament on the left side. Filaments are formed in magnetic loops that hold relatively cool, dense gas suspended above the surface of the Sun.

Credit: NASA SDO

[CamillaCorona]

A key to understanding the dynamics of the Sun and what causes the great solar explosions there relies on deciphering how material, heat and energy swirl across the Sun's surface and rise into the upper atmosphere, or corona. Tracking the constantly moving material requires state-of-the-art telescopes with the highest resolution possible. 

Observing coronal loops, which are giant arcs of solar material constrained to travel along that particular path by the magnetic fields in the sun's atmosphere, help scientists learn more about the workings of the Sun. These loops can vary in complexity over the Sun's 11-year activity cycle, becoming more or less intertwined and inter-connected. Observations of this phenomena can help researchers understand what's happening with our star's complicated magnetic fields that can also power great eruptions on the Sun such as the solar flares or coronal mass ejections.

This segment captures approx. 38 hours from December 9 to 10, 2012 and shows the 171 angstroms wavelength. This channel is particularly good for observing coronal loops. This area shows the Active Region 1629 and 1630 and their interactions with each other. Also visible is a nice flow along a filament on the left side. Filaments are formed in magnetic loops that hold relatively cool, dense gas suspended above the surface of the Sun. 

Credit: NASA SDO

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