The neutral hydrogen sheets and supergiant shells of the Large Magellanic Cloud

Details The neutral hydrogen sheets and supergiant shells of the Large Magellanic Cloud The neutral hydrogen sheets and supergiant shells of the Large Magellanic Cloud

Apr 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.225..591m&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 225, April 1, 1987, p. 591-605.

Astronomy and Astrophysics

Astronomy

30

H Lines, Magellanic Clouds, Neutral Gases, Stellar Envelopes, Supergiant Stars, Emission Spectra, Kinetic Energy, Line Shape, Radial Velocity, Stellar Winds, Supernovae

Scientific paper

Profiles of the 21-cm H I emission line have been obtained with high signal-to-noise ratios at 0°.5 intervals along three long tracks which intersect supergiant shells of the Large Magellanic Cloud. The half-power beamwidth was 14.85 arcmin. Along one of the tracks, evidence is found of extensive overlapping sheets of H I, 1 - 3 kpc across, with different radial velocities. The authors estimate that the extensive H I sheets have a total kinetic energy ≅4.5×1054erg in their motion away from the H I in the plane of the LMC. This could be supplied by supernovae and stellar winds over 2×107yr. It is interesting that tidal disruption of the LMC by the Galaxy could produce stellar motions similar to those observed in the H I sheets, but it is not clear how the sheets could form in this way. The very-high-velocity components in the vicinity of supergiant shells have kinetic energies of ≅1052erg with respect to the plane of the LMC. This energy is easily provided by a few supernovae or by stellar winds.

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