Thermodynamic models and fine structure of prominences

Details Thermodynamic models and fine structure of prominences Thermodynamic models and fine structure of prominences

Sep 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980soph...67..351e&link_type=abstract

Solar Physics, vol. 67, Sept. 1980, p. 351-355.

Physics

13

Fine Structure, Solar Prominences, Stellar Models, Brightness, H Alpha Line

Scientific paper

Observed H-alpha brightness versus size of emission substructures of quiescent prominences are compared with values predicted from thermodynamical models. The measured size of an emission element of a given brightness is substantially less than the theoretical value. Two possible causes for the discrepancy are suggested: (1) The partial filling of a recording aperture, due to the prominence fine structure, may affect the measurements seriously. Caution is therefore urged against using face values of observed brightness vs ratios in model calculations in cases of partly optically thick lines. (2) Changes of individual fine structure elements on a time scale of a few minutes implies that the prominence plasma may be in a non-stationary radiative state.

Affiliated with

Also associated with

No associations

Rating

Thermodynamic models and fine structure of prominences does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Thermodynamic models and fine structure of prominences, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Thermodynamic models and fine structure of prominences will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-908703