Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982saosr.392a.245r&link_type=abstract
In Smithsonian Astrophysics Observatory 2nd Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, Vol. 1 p 245-259 (
Astronomy and Astrophysics
Astrophysics
3
Eclipses, High Resolution, Line Spectra, Red Giant Stars, Supergiant Stars, Amplitudes, Chromosphere, Electron Density (Concentration), Excitation, K Stars, Optical Pumping, Radial Velocity
Scientific paper
32 Cyg shows a spectacular pure emission line spectrum during eclipse. Six weeks later, most lines, which were observed in emission during eclipse, are seen as P Cygni type profiles with strong absorption components. The lines are formed through line scattering of B star light in the extended atmosphere (wind) of the K supergiant. During eclipse, the emission parts of the P Cyg lines remain visible since the size of the line scattering sphere around the B star is larger than the red giant. Other emission lines are formed in a shock front near the B star (CIV, SiIV, FeIII) and possibly in an accretion disk. The strong FeII UV Mult. 191 lambda lambda 1785-88 A is shown to be formed through optical pumping via FeII UV Mult. 9 photons. The phase dependence of the P Cyg type profiles is modelled by means of line transfer calculations in nonspherical, 3-dimensional geometry with velocity fields.
Che Aixia
Hempe K.
Reimers Dieter
No associations
LandOfFree
High-resolution IUE observations of the 1981 eclipse of 32 CYG 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 High-resolution IUE observations of the 1981 eclipse of 32 CYG, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and High-resolution IUE observations of the 1981 eclipse of 32 CYG will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1648420