Quantitative spectroscopy of the HeI cluster in the Galactic center.

Details Quantitative spectroscopy of the HeI cluster in the Galactic center. Quantitative spectroscopy of the HeI cluster in the Galactic center.

Sep 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...325..700n&link_type=abstract

Astronomy and Astrophysics, v.325, p.700-708

Astronomy and Astrophysics

Astrophysics

150

Stars: Early-Type, Stars: Mass-Loss, Stars: Supergiants, Stars: Emission-Line, Galaxy: Center, Infrared: Stars

Scientific paper

We present first results on quantitative infrared spectroscopy of the brightest HeI emission line stars in the Galactic center. The observed HeI and H broad emission lines are caused by extremely strong stellar winds (˙(M)~5 to 80x10^-5^Msun_/yr) with relatively small outflow velocities (Vinfinity_~300 to 1000km/s). The effective temperatures of the objects range from 17,000K to 30,000K with corresponding stellar luminosities of 1 to 30x10^5^Lsun_. Strongly enhanced helium abundances (N_He_/N_H_>.5) are found. These results indicate that the HeI emission line stars are evolved blue supergiants close to the evolutionary stage of Wolf-Rayet stars. They power the central parsec and belong to a young stellar cluster of massive stars which formed a few million years ago.

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