Educação matemática pela arte
Gusmão, Lucimar Donizete
2013-08-28
Search results
52 records were found.
Formation of GMCs is one of the most crucial issues in galaxy evolution. I
will compare CO and HI in the LMC in 3 dimensional space for the first time
aiming at revealing the physical connection between GMCs and associated HI gas
at a ~40 pc scale. The present major findings are 1) [total CO intensity]
[total HI intensity]0.8 for the 110 GMCs, and 2) the HI intensity tends to
increase with the evolution of GMCs. I argue that these findings are consistent
with the growth of GMCs via HI accretion over a time scale of a few x 10 Myrs.
I will also discuss the role of the background stellar gravity and the
dynamical compression by supershells in formation of GMCs.
Comment: 9 pages, 8 Encapsulated Postscript figures, uses aipxfm.sty
aipproc.cls aip-6s.clo aip-8d.clo aip-8s.clo
Comment: 7 pages, 5 figures. PASJ accepted
Comment: 14 pages, 11 figures, accepted for publication in the Astrophysical
Journal
Comment: 11 pages, LaTeX uses PASJ2.sty, PASJ95.sty, PASJadd.sty 2 EPS, 5 gif,
and 1 png figures to be published in Publications of the Astronomical Society
of Japan http://www.a.phys.nagoya-u.ac.jp/~tatihara/work/research.html
Comment: To be published in PASJ Vol. 64 No.1 (February 2012)
Comment: 4 pages, 1 figure, accepted by PASJ Letters
We examine the recent star formation associated with four supergiant shells in the Large Magellanic Cloud (LMC): LMC 1, 4, 5, and 6, which have been shown to have simple expanding-shell structures. H II regions and OB associations are used to infer star formation in the last few Myr, while massive young stellar objects reveal the current ongoing star formation. Distributions of ionized H I and molecular components of the interstellar gas are compared with the sites of recent and current star formation to determine whether triggering has taken place. We find that a great majority of the current star formation has occurred in gravitationally unstable regions, and that evidence of triggered star formation is prevalent at both large and local scales.
