Evidence for supermassive stars in three Seyfert galaxy nuclei from IUE spectra

Details Evidence for supermassive stars in three Seyfert galaxy nuclei from IUE spectra Evidence for supermassive stars in three Seyfert galaxy nuclei from IUE spectra

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...297..611s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 297, Oct. 15, 1985, p. 611-620. NASA-supported research.

Astronomy and Astrophysics

Astrophysics

6

Electron Scattering, Galactic Nuclei, Iue, Seyfert Galaxies, Supermassive Stars, Ultraviolet Spectra, Kinetic Energy, Optical Thickness, Stellar Mass

Scientific paper

The variability in the ultraviolet continua and the C IV 1550 A emission profiles in the three Seyfert 1 galaxies NGC 4151, NGC 5548, and Fairall 9 are consistent with origin in supermassive stars undergoing explosive mass loss. Blackbody fits to continua of each imply a single thermal source whose area either remains constant or increases moderately as its temperature decreases, with the surface area consistent with stars having masses from 10 to the 6th to 10 to the 8th solar mass. Line emission profiles of C IV 1550 A in the same spectra are individually consistent with uniform expansion of shells of emitting gas expelled from the stars at radial velocities from 10,000 to 16,000 km/s. The kinetic energy removed by repetitive production of such massive shells approximately balances the nuclear energy production expected from supermassive stars of the indicated size. Finally, the observed nature and time scale of the variability of NGC 4151 is consistent with the relatively sudden appearance, and subsequent cooling, of the underlying superstellar surface as one such shell becomes transparent during its expansion.

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