Other
Scientific paper
Jul 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1904u&link_type=abstract
IUE Proposal ID #WRGAU
Other
Scientific paper
The binary system V444 Cygni (P = 4.212424 day) is an important object for determining the sizes and masses of 0 and WR stars. However, no spectrographic studies of its orbit have been made since 1950. The orbital elements given by Munch (1950) require confirmation, especially the elements describing the motion of the WR star. Spectrophotometric observations from the ground by Kuhi (1968) indicate that the system is enveloped in high-temperature gas which may be streaming between the stars. Review of the four (3 SWP, I LWR) high-resolution spectrograms of this system taken previously by others indicates that absorption lines attributable to the O star occur in the wavelength range from 1700 to 1900A, and that rather sharp absorption components associated with the C II resonance lines and with N IV 1718 occur on some of the spectrograms, but not on others. It is planned to follow V444 Cygni through one orbital cycle obtaining spectra throughout both eclipses and at the elongations. Observations will be made with the SWP camera using the spectrograph in the highresolution mode and with the large aperture. The resulting series of spectra will permit us to confirm and improve the orbital elements of Munch, and to track what, if any, streams of gas occur in the system. Improved orbital elements will allow us to deduce improved sizes and masses for the two stars. Analysis of the blended spectra and comparisons with the spectra of single stars having equivalent spectral types to those of the components of V444 Cygni will allow us to infer information about the physical state of the atmosphere of each star. Appropriate comparison spectra of single stars exist in NSSDC. The P.I. has copies of some of them.
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