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2009MNRAS.399.2004M - Mon. Not. R. Astron. Soc., 399, 2004-2020 (2009/November-2)
Effects of ram pressure on the gas distribution and star formation in the Large Magellanic Cloud.
MASTROPIETRO C., BURKERT A. and MOORE B.
Abstract (from CDS):
Due to the present nearly edge-on orientation of the disc with respect to the orbital motion, compression at the leading edge can explain the high density region observed in Hi at the south-east border. In the case of a face-on disc (according to Mastropietro the LMC was moving almost face-on before the last perigalactic passage), ram pressure directed perpendicular to the disc produces a clumpy structure characterized by voids and high density filaments that resemble those observed by the Parkes Hi survey. As a consequence of the very recent edge-on motion, the Hα emission is mainly concentrated on the eastern side where 30 Doradus and most of the supergiant shells are located, although some Hα complexes form a patchy distribution on the entire disc. In this scenario, only the youngest stellar complexes show a progression in age along the leading border of the disc.
Abstract Copyright: © 2009 The Authors. Journal compilation © 2009 RAS
Journal keyword(s): hydrodynamics - methods: {em N}-body simulations - galaxies: individual: LMC - galaxies: interactions
Simbad objects: 11
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