Wind and Fuv Flux Variability in X-Ray Emitting Be Stars

Monthly IUE observations of classical Be stars which were detected as X-ray sources in the Uhuru database are proposed to explore the possibility that the X-rays are associated with the presence of very high velocity (<-800 km s^-1) narrow components (VHVNC) in the wind lines and investigate the cause for variability observed in their FUV flux and winds. A correlation between X-ray emission and VHVNCs would suggest a common line formation region for both. Presently there is circumstantial evidence for this as many of the Uhuru sources have shown transient narrow components with expansion velocities in excess of 1000 km s^-1. Both X-ray emission and VHVNCs are rarely observed in the general population of classical Be stars. As the Uhuru Be stars are likely to be detected in the ROSAT all sky survey, IUE coverage will allow us to answer the question about the possible X-rayVHVNC connection. Voyager UVS and IUE observations have revealed that the FUV flux (900-1200 A) and winds vary in most of the X-ray emitting Be stars. The VHVNC in the wind tend to be transient. I propose IUE and Voyager observations of these objects before and after the ROSAT coverage to investigate the pre- and posthistory of the wind and continuum activity. This will allow us to assess whether the X-ray generation is a function of earlier/later high energy events in the wind/photosphere, even if VHVNCs are not observed contemporaneously with the Xrays. Program stars include gamma Cas, 48 Per, HR 4009, kappa Dra, pi Aqr (all of which were detected in the Uhuru database and lambda Eri, 66 Oph, and 59 Cyg, which were not found to be hard X-ray sources but frequently show VHVNCs.