[Previous] | [Session 53] | [Next]
H. Uitenbroek (NSO/Sac Peak)
The dark cores of infrared rotation-vibration lines of the CO molecule that are observed close to the solar limb pose a major difficulty for for efforts to model the solar chromosphere as one-dimensional hydrostatic layer. If temperatures are allowed to go well below 4000K as seems to be required by the CO lines, the reulting intensities in the UV continua and in the Ca II resonance lines turn out to be much lower than observed. I will discuss the severe constraints that the CO lines pose on the one-dimensional semi-empirical modeling, and discuss possible solutions in terms of multi-dimensional structure and/or time dependent models. In both types of models the spectrum is averaged in a non-linear way because of the way the formation height of radiation is affected by the conditions in the plasma. This provides ways for the plasma to exhibit both the qualities of hot and cold temperatures at the same time in the case of spatial inhomogeneities, or on average in case of time-dependent conditions.
If you would like more information about this abstract, please follow the link to http://www.nso.edu/~uitenbr. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.
The author(s) of this abstract have provided an email address for comments about the abstract: huitenbroek@nso.edu
[Previous] | [Session 53] | [Next]
Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.