A Brightening Coronal Loop Observed by TRACE. I. Morphology and Evolution

Details A Brightening Coronal Loop Observed by TRACE. I. Morphology and Evolution A Brightening Coronal Loop Observed by TRACE. I. Morphology and Evolution

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...535..412r&link_type=abstract

The Astrophysical Journal, Volume 535, Issue 1, pp. 412-422.

Astronomy and Astrophysics

Astronomy

28

Sun: Activity, Sun: Corona, Sun: X-Rays, Gamma Rays

Scientific paper

We analyze the transient brightening of a solar coronal loop observed, at high time cadence (30 s) and spatial resolution (0.5" pixel size), with the Transition Region and Coronal Explorer (TRACE) in the 171 Å band on 1998 June 26. The loop, located in AR 8253, is ~1010 cm long and inclined with respect to the vertical to the solar surface. Its geometry and shape do not change significantly during the brightening, which lasts for ~2 hr and is preceded by highly dynamic events in nearby and perhaps interacting loops. The loop footpoints brighten first; after ~10 minutes, moving brightness fronts rise initially from the northern footpoint, and after another ~7 minutes from the southern one, at an apparent speed ~100 km s-1, the whole loop becoming clearly visible afterward. During the rising phase the loop evolves coherently as a single magnetic tube. The brightness profile is asymmetric with respect to the loop apex at all times; the brightness contrast between the footpoints and the apex decreases with time from a ratio of ~10 to ~3. After the loop has become all visible, the several parallel filaments which form it follow an independent evolution. Assuming a plasma temperature of ~1 MK, we infer a plasma density of ~6×108 cm -3 and a pressure of ~0.2 dyn cm-2 close to the loop apex at the luminosity maximum. A companion paper is devoted to modeling the rising phase of this event.

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