Spatial and temporal variations of solar coronal loops

Details Spatial and temporal variations of solar coronal loops Spatial and temporal variations of solar coronal loops

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...98..323h&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 98, Aug. 1985, p. 323-340.

Physics

28

Coronal Loops, Solar Limb, Extreme Ultraviolet Radiation, Skylab Program, Spatial Distribution, Temporal Distribution

Scientific paper

Skylab EUV observations of an active region near the solar limb were analyzed. Both cool (T < 106K) and hot (T > 106K) loops were observed in this region. For the hot loops the observed intensity variations were small, typically a few percent over a period of 30 min. The cool loops exhibited stronger variations, sometimes appearing and disappearing in 5 to 10 min. Most of the cool material observed in the loops appeared to be caused by the downward flow of coronal rain and by the upward ejection of chromospheric material in surges. The physical conditions in the loops (temperatures, densities, radiative and conducting cooling rates, cooling times) were determined. On a coronal heating mechanism that can account for the observed behavior of the EUV emission from McMath region 12634 is heating by the dissipation of fast mode MHD waves.

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