UV absorption toward 8 LMC stars shows redshifted gas near 30 Doradus that appears to trace the Magellanic arms B and E on the near side of the LMC, extending about 1 degree further than previously mapped.
Bow-shock induced star formation in the LMC?
1 Pith paper cite this work, alongside 4 external citations. Polarity classification is still indexing.
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abstract
The structure of supergiant shells, in particular of LMC 4, is hard to explain with stochastic self-propagating star formation. A series of supergiant structures lies along the outer edge of the LMC and form a sequence increasing clockwise in age. We have considered the rotation of the LMC and its motion through the halo of the Milky Way and propose that these structures find their origin in star formation induced in the bow-shock formed at the leading edge of the LMC. Due to the rotation of the LMC these structures then move aside.
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New Interpretation for the Orientation of the LMC's Gaseous Arms B and E using ULLYSES
UV absorption toward 8 LMC stars shows redshifted gas near 30 Doradus that appears to trace the Magellanic arms B and E on the near side of the LMC, extending about 1 degree further than previously mapped.