Abstract
THE EFFECTS of higher surface gravity on flux distribution and line blanketing are most easily studied by a comparison of main sequence stars and white dwarfs in the two-colour diagram. As can be seen from EGGEN and GREENSTEIN’S observational material”’ the white dwarfs are located much closer to the black-body line in the (U-B, B-V) plane. Following ARP(~) who demonstrated how deviations from the black-body line are caused by the effects of (a) non-greyness of the continuous opacity and (b) line blanketing one could presume the white dwarfs to be more similar to grey or black bodies since higher pressure tends to smooth the opacity distribution whereas the observed fact that white dwarf spectra are generally line-poor’3’ renders blanketing unimportant. Although this is partly true (especially for spectral type DC, without any lines*) it will be shown in the present note that blanketing effects are in most cases far from negligible and must be considered in order to understand the observed UBV-distribution.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
