Starting in the 1960's at the Mt. Wilson Observatory O.C. Wilson (sic) began a long - term study of magnetic cycles in cool stars using as his observational indicator
the variable emission flux of the H and K resonance lines of ionized calcium whose appearance in emission is characteristic of stellar chromospheres.
Not exact matches
The
flux estimates presented in previous sections use available estimates from every reservoir where GHG
emissions have been reported (and mean estimates from reservoirs where multiple studies or years of data have been collected), but it is important to note that the spatial and temporal coverage of these
emission estimates are highly
variable.
At the characteristic -
emission level, ZC, the
variable altitude at which incoming and outgoing radiative
fluxes balance, TC ≈ 254 ° K, so that κC ≈ 0.269 ° K W — 1 m2.