The expansive motions of the giant shells in the N44 (DEM 150, 151, 152) interstellar complex in the Large Magellanic Cloud

Details The expansive motions of the giant shells in the N44 (DEM 150, 151, 152) interstellar complex in the Large Magellanic Cloud The expansive motions of the giant shells in the N44 (DEM 150, 151, 152) interstellar complex in the Large Magellanic Cloud

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...245..635m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 245, no. 2, May 1991, p. 635-642.

Astronomy and Astrophysics

Astrophysics

20

Interstellar Matter, Magellanic Clouds, Stellar Winds, Supernova Remnants, Cosmic Gases, Stellar Envelopes

Scientific paper

Eechelle observations of H-alpha profiles reveal that the near-side of the primary 70 x 50 pc diameter giant shell in the N44 complex (Shell 1) is expanding towards the observer at 46 km/s and the far-side is expanding away at 33 km/s with respect to 307 km/s heliocentric radial velocity. Two components with heliocentric radial velocities at 287 and 307 km/s are found in the Na I interstellar absorption line profiles in the light of stars in the Ob association, LH47, enclosed by Shell 1. These components are shown to originate in the extensive clouds of the LMC gas out of which the N44 complex formed. Four independent methods are used to show that a Lyman photon rate from equivalent to 10 + or - 5 O5-type supergiant stars is needed to radiatively ionize the N44 complex. If the supernova rate in LH 47 is proportional to the Lyman flux to give 280 + or - 140 explosions in 3.5 x 10 to the 6th yr, the Shell 1 must be a momentum-conserving snowplough.

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