Yn. Efremov et Bg. Elmegreen, TRIGGERED STAR-FORMATION IN THE LMC4 CONSTELLATION-III REGION OF THE LARGE-MAGELLANIC-CLOUD, Monthly Notices of the Royal Astronomical Society, 299(3), 1998, pp. 643-652
The origin of a regular, 600-pc-long are of young stars and clusters i
n the Constellation III region of the Large Magellanic Cloud is consid
ered. The circular form of this are suggests that the pre-stellar gas
was uniformly swept up by a central source of pressure. In the centre
of the are are six similar to 30-Myr-old A-type supergiant stars and a
Cepheid variable of similar age, which may be related to the source o
f this pressure. We calculate the expansion of a bubble around a clust
er of this age, and show that it could have triggered the formation of
the are at the right time and place. Surrounding the central old star
s and extending well outside the young are is the LMC4 superbubble and
giant H I shell. We show how this superbubble and shell could have fo
rmed by the continued expansion of the 15-Myr-old cavity, following st
ar formation in the are and the associated new pressures. The age sequ
ence proposed here was not evident in the recent observations by Olsen
et al. and Braun et al, because the first generation stars in the cen
tre of the LMC superbubble are relatively faint and scarce compared to
the more substantial population of stars less than 15 Myr old that fo
rmed throughout the region in a second generation. These consideration
s lead to an examination of the origin of the LMC4/Constellation III r
egion and other large rings in the LMC and other galaxies. Their size
and circularity could be the result of low galactic shear and a thick
disc, with several generations of star formation in their interiors no
w too faint to be seen.