1999A&AS..136...95R

We discuss new and archive spectroscopic and photometric observations of the Herbig Ae star V380 Ori obtained between 1978 and 1995 and covering at different epochs the wavelength range from 1200Å to 5µm. The coordinated JHKLM and CVF infrared observations and optical spectroscopy made at ESO of March 1985 confirm the presence of a strong IR excess due to emission from hot cicumstellar dust. The comparison with IR photometry from the literature suggests the presence of oscillations, without secular variations. The optical spectrum of V 380 Ori, observed at ESO during 1983-1985, and at OHP in January 1995, remained substatially stable, and was all the time characterized by a large number of broad (FWHM∼150km/s) permitted emission lines, probably formed in a rotating optically thick disk. The strongest FeII lines have complex profile with a principal central emission and a blue-shifted (-140km/s) wind component, the redward component probably being occulted by the disk. The multiplet 42 lines have P Cygni absorption components shifted by -250km/s which should be associated with a teneous cool wind. We remark the secular behaviour of the stellar activity probe HeI 5876Å line, which is present in all our spectra as a broad emission, while in other times it was absent or in absorption. The ultraviolet (IUE) spectrum shows a short wavelength cut off at ∼1300Å typical of a B9-A0 star, with a rich absorption spectrum, which is thought to be produced in an optically thick stellar envelope or wind. The 2175Å interstellar band strength is consistent with a mean galactic-type extinction law with an E_B–V=0.20±0.05, much smaller than that derived from the visual (∼0.5), which suggests an anomalous local UV extinction. The comparison of the archive IUE data shows that during 1978-1989 there was no significant flux variation, with the possible exception of the UV MgII emission line.