The fine structure of H110-alpha-line emission in the Orion nebula

Details The fine structure of H110-alpha-line emission in the Orion nebula The fine structure of H110-alpha-line emission in the Orion nebula

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992sval...18..100g&link_type=abstract

Soviet Astronomy Letters, Vol. 18, p. 100; Pis'ma v Astronomicheskii Zhurnal (ISSN 0320-0108), vol. 18, no. 3, March 1992, p. 24

Astronomy and Astrophysics

Astronomy

Emission Spectra, Fine Structure, H Alpha Line, Orion Nebula, Antenna Radiation Patterns, Isophotes, Radio Astronomy, Radio Telescopes

Scientific paper

The morphology of H110-alpha-line emission was obtained with the RATAN-600 radio telescope with a resolution of 40 arcsec x 6 arcmin x 9.7 km/s. Observations revealed that the core of the nebula has a small rotation, and that there is a thin envelope with a diameter of 0.36 pc expanding with velocities of +40 and -70 km/s. The distribution of the electron temperature across the nebular disk confirms the idea that this envelope is the result of the action of stellar wind from the star Theta-1C Orionis. The kinematic parameters of the envelope and the remaining gas show that the age of Theta-1C is about 2000 yr, while less bright stars appeared about 30,000 yr ago.

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