An Assessment of Coronal Heating Models based on Yohkoh, SoHO, and TRACE Observations

Details An Assessment of Coronal Heating Models based on Yohkoh, SoHO, and TRACE Observations An Assessment of Coronal Heating Models based on Yohkoh, SoHO, and TRACE Observations

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sp61a08a&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SP61A-08

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy, 7507 Chromosphere, 7509 Corona, 7546 Transition Region

Scientific paper

Recent soft X-ray and EUV data from space observations with Yohkoh, SoHO, and TRACE established three important observational constraints for coronal heating models: (1) Coronal loops have an overdensity that can only be supplied by upflows of heated chromospheric plasma, (2) chromospheric upflows have been observed in a large number of coronal loops, and (3) the coronal heating function has been localized in the lower corona within a height range of λH <~ 10-20 Mm above the photosphere. We discuss and compare a comprehensive set of theoretical models on coronal heating under the aspect whether they can satisfy these observational constraints. We find that conventional DC and AC coronal heating models that consider coronal loops as homogeneous flux tubes (in density and temperature), detached from the transition region, do not predict these observed effects, while refined models that include gravity and chromospheric models can reproduce the observed effects. Alternatively, most of the magnetic reconnection models previously used for flares, can reproduce the observed effects, because heating of the chromospheric plasma at the loop footpoints is involved with subsequent chromospheric evaporation like in flares. Therefore, coronal magnetic reconnection processes that work with lower heating efficiency than in flares, as well as chromospheric and photospheric reconnection processes should be considered as serious candidates for coronal heating models. Our main conclusion is that the coronal heating problem cannot be solved without including dynamic processes (and related heating effects) in the chromosphere and transition region zone.

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