Kinematics of ring-shaped nebulae in the LMC. II - The radial velocity field of N 185

Details Kinematics of ring-shaped nebulae in the LMC. II - The radial velocity field of N 185 Kinematics of ring-shaped nebulae in the LMC. II - The radial velocity field of N 185

Nov 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...115...61r&link_type=abstract

Astronomy and Astrophysics, vol. 115, no. 1, Nov. 1982, p. 61-64.

Astronomy and Astrophysics

Astrophysics

23

Astronomical Spectroscopy, Interstellar Matter, Kinematics, Magellanic Clouds, Nebulae, Radial Velocity, Ring Structures, Spectral Energy Distribution, Supernova Remnants

Scientific paper

The LMC ring-shaped nebula N 185 is studied by means of H-alpha and forbidden S II imagery and Fabry-Perot interferometry. From an investigation of the stellar content, it is shown that the interior stars can photoionize the nebula. This finding, together with the results from the H-alpha imagery, makes it possible to derive an electron density of about 4/cu cm for the shell. It is also found that the forbidden S II (6717)/H-alpha ratio varies from 0.15 to 0.4 among different filaments. This variation can be understood by considering differences in the degree of ionization. The radial velocity field can be accounted for by an expansion of 70 km/s plus or minus 10 km/s superimposed on a systematic motion of 262 plus or minus 11 km/s. The resulting parameters make it possible to distinguish different origins of this expanding shell. A supernova explosion, it is noted, is more adequate for explaining the energetics of the nebula than stellar winds from the present star.

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