The temperature and dynamics of the ionized gas in the nucleus of our Galaxy

Details The temperature and dynamics of the ionized gas in the nucleus of our Galaxy The temperature and dynamics of the ionized gas in the nucleus of our Galaxy

Mar 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...228..734r&link_type=abstract

Astrophysical Journal, Part 1, vol. 228, Mar. 15, 1979, p. 734-739.

Astronomy and Astrophysics

Astronomy

21

Galactic Nuclei, Gas Dynamics, Gas Temperature, Ionized Gases, Milky Way Galaxy, Radio Sources (Astronomy), Abundance, Astronomical Models, H Alpha Line, H Beta Line, Halos, Infrared Spectra, Kepler Laws

Scientific paper

Observations of the H65-alpha (23.4 GHz), 484-alpha (10.9 GHz), and H94-alpha (7.8 GHz) radio recombination lines from Sgr A West are presented. It is suggested that a core-halo model can satisfactorily account for the reported radio and infrared observations of this source. Due to instrumental limitations, the observed infrared lines are dominated by the core, while the observed radio radiation arises mostly in the halo. Although more than a factor of 10 brighter than the halo, the core is responsible for only about one-fourth of the integrated thermal continuum from Sgr A West. The proposed model implies that the neon abundance determination from infrared observations, previously considered consistent with the solar value, should be revised upward by a factor of 4. This suggested enrichment of neon relates strongly to the derivation of an unusually low electron temperature, + or - 1000 K, since nebular cooling is expected to be enhanced by an overabundant heavy-element content. The dynamical structure of Sgr A West can be explained in terms of Keplerian rotation due to the gravitational field of the normal stellar population plus a central mass point of 5 million solar masses.

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