Low and high dispersion ultraviolet spectra were obtained of the Ml supergiant TV Gem with IUE. Previous IUE observations of this late type supergiant revealed unexpected W continuum emission, perhaps arising from an early B companion. Low resolution spectra obtained approximately one year apart suggest that the strong Si I11 in-combination perhaps with 0 I at wavelengths % A1300 A varies considerably with time. Large variation the column density is required to explain these changes. Sporadic mass expulsion with mass loss rates dM/dt * 10-5 S y r - l from the M supergiant could lead to a dense circumstellar wind near the hot early companion, and thus could account for these observed variations in equivalent width. The high resolution spectrum in the A2000 to 3200 A wavelength range is characterized by narrow absorption lines primarily due to Fe 11, Mn I1 and Mg I1 (h and k), which are skewed in profile with an extended red wing, We tentatively attribute this profile structure to interstellar absorption and an intervening differentially moving cloud in the direction of Gem OB1, of which TV Gem is a known association member.
IUE, UV, ultraviolet, M1, Supergiant, TV Gem, TV Gemini
Instrumentation | Stars, Interstellar Medium and the Galaxy
Michalitsianos, A.G., Kafatos, M. (1982). UV emission from the M1 supergiant TV Gem. In Y. Kondo, J.M. Mead, & R.D. Chapman (Eds.), Advances in Ultraviolet Astronomy: Four Years of IUE Research. Proceedings of a Symposium held at NASA Goddard Space Flight Center, Greenbelt, Maryland, March 30-April 1, 1982 (pp. 263-267).