Supermassive stars in galactic nuclei

Details Supermassive stars in galactic nuclei Supermassive stars in galactic nuclei

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...158..367k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 158, no. 1-2, April 1986, p. 367-370.

Astronomy and Astrophysics

Astrophysics

5

Galactic Nuclei, Stellar Evolution, Supermassive Stars, Galactic Bulge, Infrared Spectra, Main Sequence Stars, Stellar Luminosity, Stellar Mass Accretion, Stellar Spectra, Stellar Winds

Scientific paper

The framework of a simple analytical model supermassive stars (SMS) in the mass range between 1000 and about 500,000 solar masses is discussed. An SMS is expected to possess a strong stellar wind and, if it is located in the potential well of a galactic nucleus, a high accretion rate fed by mass loss from the old stars in the galactic bulge is also very likely. The coexistence of accretion and a strong stellar wind can theoretically lead to an 'eternal' SMS, where accretion occurs from a disk and mass loss into all other directions. The IR spectra is also presented of an SMS with luminosity of 3 x 10 to the 8th solar luminosities buried in a dust medium closely resembling the inner 300 pc of the Galactic center. From comparison of these spectra with observations of the Galactic center, it is concluded that an SMS of such a luminosity cannot be responsible for either the ionizing flux or for the IR emission. However, a less luminous SMS (less than or equal to 10 to the 8th solar luminosities) cannot be excluded as an additional source of energy and ionization.

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