On the nature of the Herbig Be star V 380 Orionis

Details On the nature of the Herbig Be star V 380 Orionis On the nature of the Herbig Be star V 380 Orionis

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26as..136...95r&link_type=abstract

Astronomy and Astrophysics Supplement, v.136, p.95-105

Astronomy and Astrophysics

Astrophysics

14

Stars: Emission-Line, Be, Stars: Individual: V 380 Ori, Stars: Pre-Main Sequence, Infrared: Stars, Ultraviolet: Stars

Scientific paper

We discuss new and archive spectroscopic and photometric observations of the Herbig Ae star V 380 Ori obtained between 1978 and 1995 and covering at different epochs the wavelength range from 1200 Angstroms to 5 mu m. 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 ~ 150 km s(-1) ) permitted emission lines, probably formed in a rotating optically thick disk. The strongest Fe Ii lines have complex profile with a principal central emission and a blue-shifted (-140 km s(-1) ) wind component, the redward component probably being occulted by the disk. The multiplet 42 lines have P Cygni absorption components shifted by -250 km s(-1) which should be associated with a teneous cool wind. We remark the secular behaviour of the stellar activity probe He I 5876 Angstroms 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 ~ 1300 Angstroms 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 2175 Angstroms \ 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 Mg Ii emission line. Based on observations made with the International Ultraviolet Explorer collected at the Villafranca Satellite Tracking Station of ESA, on archive IUE data, and on observations collected at the European Southern Observatory, at the Observatoire de Haute Provence. Table 3 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html

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