MORA A., EIROA C., NATTA A., GRADY C.A., DE WINTER D., DAVIES J.K., FERLET R., HARRIS A.W., MIRANDA L.F., MONTESINOS B., OUDMAIJER R.D., PALACIOS J., QUIRRENBACH A., RAUER H., ALBERDI A., CAMERON A., DEEG H.J., GARZON F., HORNE K., MERIN B., PENNY A., SCHNEIDER J., SOLANO E., TSAPRAS Y. and WESSELIUS P.R.
Abstract (from CDS):
We present high resolution (λ/Δλ=49000) echelle spectra of the intermediate mass, pre-main sequence stars BF Ori, SV Cep, WW Vul and XY Per. The spectra cover the range 3800-5900Å and monitor the stars on time scales of months and days. All spectra show a large number of Balmer and metallic lines with variable blueshifted and redshifted absorption features superimposed to the photospheric stellar spectra. Synthetic Kurucz models are used to estimate rotational velocities, effective temperatures and gravities of the stars. The best photospheric models are subtracted from each observed spectrum to determine the variable absorption features due to the circumstellar gas; those features are characterized in terms of their velocity, v, dispersion velocity, Δv, and residual absorption, Rmax. The absorption components detected in each spectrum can be grouped by their similar radial velocities and are interpreted as the signature of the dynamical evolution of gaseous clumps with, in most cases, solar-like chemical composition. This infalling and outflowing gas has similar properties to the circumstellar gas observed in UX Ori, emphasizing the need for detailed theoretical models, probably in the framework of the magnetospheric accretion scenario, to understand the complex environment in Herbig Ae (HAe) stars. WW Vul is unusual because, in addition to infalling and outflowing gas with properties similar to those observed in the other stars, it shows also transient absorption features in metallic lines with no obvious counterparts in the hydrogen lines. This could, in principle, suggest the presence of CS gas clouds with enhanced metallicity around WW Vul. The existence of such a metal-rich gas component, however, needs to be confirmed by further observations and a more quantitative analysis.