A standard method for evaluating the abundances of chemical species in stellar atmospheres is the COG. Assuming a species concentration fixed with depth, the theory of the COG evaluates the equivalent width of a spectral line as a function of the concentration times the transition probability of the line. The classical method is based on a single line, which is far from being the case in when multiple molecular lines are present. Hence a substantial modification is called for. Moreover, the commonly used COG method does not take into account a variable concentration with height, as trace gases may show.
The technology, a platform remote sensing for determining the vertical temperature profile and the 3D distribution of atmospheric components within a given planetary atmosphere, using a novel curve of growth calculation based on data retrieved from remote sensing.
- May be used to identify the spectral data in spectra as required for radiative transfer calculations
- Allows understanding of the physics and chemistry of spectrally structured radiative sources
- Data reduction from spectral databases can be done without losing information
Applications and Opportunities
- Abundances of chemical species in stellar atmospheres