Dynamics of the supergiant shell LMC 2 in the Large Magellanic Cloud

Details Dynamics of the supergiant shell LMC 2 in the Large Magellanic Cloud Dynamics of the supergiant shell LMC 2 in the Large Magellanic Cloud

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...110..185c&link_type=abstract

Astronomy and Astrophysics, vol. 110, no. 2, June 1982, p. 185-197. Research supported by the Delegation Generale a la Recherch

Astronomy and Astrophysics

Astrophysics

46

Gas Ionization, Magellanic Clouds, Stellar Envelopes, Velocity Distribution, H Alpha Line, H Ii Regions, Hydrogen Atoms, Interstellar Matter, Kinematics, Radial Velocity, Stellar Winds

Scientific paper

The velocity field of LMC2 was derived from 16 H-alpha photographic Fabry-Perot interferograms; 967 radial velocities were obtained over the ionized filaments and the nearby giant H II regions. The lowest velocities (230-250 km/s) are observed in the eastern and southern filaments, while the highest velocities (270-285 km/s) are observed in the central and northwestern regions. This velocity field can be explained by the expansion of a portion of a spherical shell of radius 475 pc, with a velocity of 30 km/s in an ambient neutral medium at 245 km/s. Estimates of the power currently available in the stellar winds emitted by stars located inside LMC2, and of the power likely to have been liberated by supernova explosions since the formation of LMC2, indicate that LMC2 may result from the combined action of stellar winds and supernova explosions; its age would then be approximately 10-million years.

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