Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26as..144..379m&link_type=abstract
Astronomy and Astrophysics Supplement, v.144, p.379-389
Astronomy and Astrophysics
Astrophysics
4
Stars: Emission-Line, Stars: Supergiants, Circumstellar Matter, Stars: Mass-Loss, Stars: Individual, As 314
Scientific paper
We present the results of our observations of the poorly-studied emission-line star AS 314 which include high-resolution spectroscopy, obtained at the 6 -meter telescope of the Russian Academy of Sciences, multicolor optical and near-infrared photometry. The strong Hα line, Hβ and Hγ of moderate strength and a number of weak Fe ii lines were detected in emission. The Balmer lines and most of the Fe ii lines show narrow P Cyg-type profiles which implies a very low terminal velocity of the stellar wind. Very weak signs of emission are found in Hdelta . Photospheric lines detected for the first time allowed us to determine the object's spectral type, A0. The luminosity, M_bol ~ -8.0 mag was estimated using several methods and implies that AS 314 is a hypergiant, which is located at about 10 kpc from the Sun and has an initial mass of ~ 20; Msun . Modeling of the Balmer line profiles resulted in the following parameters of the stellar wind: dot {M} = 2\ 10-5;Msun yr-1, v_infty = 75;km s-1. The star is located within the LBV strip in the HRD. Its noticeable far-IR excess is due to the circumstellar dust emission and is likely evidence of an LBV-type outburst in the past. Table 5 is only available in electronic form in the online edition of the present issue.
Chentsov Eugene L.
Klochkova Valentina G.
Miroshnichenko Anatoly S.
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