Spectroscopic orbits for symbiotic stars. I - The recurrent nova T Coronae Borealis

Properties and nature of Be stars

“…Harmanec (2001) recently pointed out that any disturbance of the true orbital RV curve which is symmetric with respect to the line joining the binary components will lead to such an effect. This is indeed observed, for instance for stars nearly filling their Roche lobes (see, e.g., Kenyon & Garcia 1986). Therefore -although there must certainly exist binaries with truly eccentric orbits and values of the longitude of periastron close to either 90 • or 270 • -one should always investigate such cases carefully against possibly spurious eccentricity.…”

The Discovery of a Companion to the Lowest Mass White Dwarf

“…We solve for the best-fit orbit using the code of Kenyon & Garcia (1986). We find that the heliocentric radial velocities of the WD are best fitted with a circular orbit and a radial velocity amplitude K ¼ 148:8 AE 6:9 km s À1 .…”

The nature of ultraviolet spectra of AG Pegasi and other symbiotic stars: locations, origins, and excitation mechanisms of emission lines

“…This should be noticed since EG And also has a region where the winds from the two stars collide (Tomov 1995). More surprising are the broad lines in T CrB and CH Cyg, since the white dwarf in these systems is known to be accreting matter from the red-giant wind (Iijima 1982;Kenyon & Garcia 1986), and therefore no whitedwarf wind is expected. The argument of matter falling into the disk surrounding the white dwarf is further strengthened here as inverted P Cygni profiles are observed in the lines C IV λ1548 (both systems) and He II λ1640 (only in T CrB).…”

“…The hot components are dominantly white dwarfs in both the S and D type systems. However, a few exceptions have the hot component as an accreation disk around a main sequence star (Kenyon & Garcia 1986).…”