Computer Science
Scientific paper
Apr 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997kfnt...13b..46p&link_type=abstract
Kinematika i Fizika Nebesnykh Tel, vol. 13, p. 46
Computer Science
A Stars, Stellar Structure, Variable Stars, Stellar Spectra, H Lines, Line Shape, Spectrum Analysis, Stellar Composition
Scientific paper
It is shown that the irregular Is(A)-type variable star V351 Ori, which may be formally classified as a young Herbig Ae star, is actually an object that left the main sequence and at present has a number of characteristics in common with the evolved objects. The conclusion is based on an analysis of echelle spectra of moderate (R = 3000) and high (R = 25,000) resolution obtained with a 6-m telescope in 1989-1991. We show that the star seems to be a slow rotator (vsini = 87.3 km/s), and its space velocity vector direction (vsp = 24.5 km/s) exludes any possibility for the star to be in the past genetically connected with the star formation region in Orion. There is an expanding emission envelope around the star, with an expanding velocity near 120 km/s and H-alpha luminosity of the envelope of about 10 exp 24 J/s. In spite of the narrow hydrogen lines, the previous classification as A7 III is confirmed while the narrow hydrogen line profiles fit better for A8 Ia. The discrepancy between small Balmer line equivalent widths and spectral class A7 III is explained by low hydrogen abundance. A conclusion has been drawn that the whole group of Herbig Ae stars is nonhomogeneous and includes objects of different evolutionary statuses.
Koval'Chuk G. U.
Pugach A. F.
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