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Spectra that cover 0.63 - 0.69um with a spectral resolution ~ 17000 arepresented of the W Serpentis system V367 Cygni. Absorption lines of FeII andSiII that form in a circumsystem shell are prominent features, and the depthsof these are stable with time, suggesting that the shell is smoothlydistributed and well-mixed. Further evidence of uniformity comes from modestradial velocity variations measured in the deepest parts of the shell lines. Itis suggested that motions previously attributed to rotation of the shell areinstead artifacts of contamination from the donor star spectrum. A donor starspectrum is extracted that is consistent with that of an early to mid-A giant.The depths of metallic lines in the donor spectrum vary with orbital phase,suggesting that spot activity covers a large fraction of the surface of thatstar. A spectrum of the accretion disk that surrounds the second star is alsoextracted, and similarities are noted with the emission spectra of Herbig Ae/Bestars. In addition to variations with orbital phase, H$\alpha$ changes withtime over timescales of no more than two orbits. A tentative detection of HeI6678 emission is made near primary minimum, but not at other phases. Finally,projected emission from hot dust in and around V367 Cyg is more-or-lesssymmetric and extends over 28 arcsec, or 0.09 pc at the distance of the system-- V367 Cyg is thus expelling matter into a large volume of the surroundingspace.

Coaxing the Eclipsing Binary V367 Cygni Out of Its Shell