The morphology and dynamics of the halo of the 30 Doradus Nebula

Details The morphology and dynamics of the halo of the 30 Doradus Nebula The morphology and dynamics of the halo of the 30 Doradus Nebula

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...117..265c&link_type=abstract

Astronomy and Astrophysics, vol. 117, no. 2, Jan. 1983, p. 265-271.

Astronomy and Astrophysics

Astrophysics

25

Hydrogen Clouds, Ionized Gases, Magellanic Clouds, Nebulae, Radial Velocity, Stellar Winds, Astronomical Photography, Fabry-Perot Interferometers, Galactic Structure, H Alpha Line, Interstellar Gas, Kinematics, Star Distribution

Scientific paper

The halo of the 30 Doradus Nebula is thought to be formed of empty ionized "shells". A Perot-Fabry interferometer, with high spectral resolution, has been used to obtain the velocity field of this region. This velocity field is clearly correlated with the morphology of the nebula: a systematic splitting of the Hα line is found inside the shells, whereas the line is single in the direction of the bright filaments surrounding the shells. These results are consistent with the interpretation of 30 Doradus as formed of expanding ionized shells, resulting from the interaction of the prevailing stellar wind emitted by R 136 with a dense interstellar medium.

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