The L1448 Molecular Cloud: Where (and why) do Stars form?

Details The L1448 Molecular Cloud: Where (and why) do Stars form? The L1448 Molecular Cloud: Where (and why) do Stars form?

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21334704k&link_type=abstract

American Astronomical Society, AAS Meeting #213, #347.04; Bulletin of the American Astronomical Society, Vol. 41, p.483

Astronomy and Astrophysics

Astronomy

Scientific paper

We apply a novel hierarchical structure identification approach (i.e., dendrograms) to the L1448 molecular cloud. This reveals that a network of dense filaments pervades the L1448 cloud and constitutes about 1/4 of the cloud's mass. Within the filaments, dense cores and stars form only in unusually massive and dense regions of high pressure that are typically influenced by strong self-gravity. Thus, one may expect that the evolution of dense cores in L1448 is primarily set by these boundary conditions (e.g., pressure and density). We find, however, that further agents matter. Dense cores seem to be also shaped the the impact of "winds" (e.g., from stars). Most interestingly, all of the dense core and star formation in L1448 might have been triggered by the collision of filaments within the cloud.

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