HIGH-DISPERSION H-ALPHA-SPECTROSCOPY OF EPSILON-AURIGAE

Halpha spectroscopic observations have been made by using a high-dispe rsion and high-resolution thick CCD system, when the orbital phase of epsilon Aur was near 0.3. During two years of out-of-eclipse observati ons, the Halpha profile varied significantly. The circumstellar gas ci rcling the F0 supergiant is possibly a ring-like H II structure, which consists of moving gaseous clouds. Halpha profile variation outside e clipse may be due to the apparent motion of gaseous clouds within the ring following the rotation of the primary, and to its intrinsic physi cal changes.