Core expansion in young star clusters in the Large Magellanic Cloud

Details Core expansion in young star clusters in the Large Magellanic Cloud Core expansion in young star clusters in the Large Magellanic Cloud

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...347l..69e&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 347, Dec. 15, 1989, p. L69-L71.

Astronomy and Astrophysics

Astrophysics

53

Globular Clusters, Gravitational Collapse, Magellanic Clouds, Astronomical Models, Expansion, Stellar Cores, Stellar Mass Ejection

Scientific paper

The core radii of 18 rich star clusters in the LMC with ages from 10 Myr to 1 Gyr. Data for an additional 17 clusters with ages from 1 Myr to 10 Gyr are available in the literature. The combined sample shows that the core radii increase from about 0 to about 5 pc between about 1 Myr and 1 Gyr, and then begin to decrease again. The expansion of the cores is probably driven by mass loss from evolving stars. Models of cluster evolution show that the rate of increase in core radius is sensitive to the slope of the initial mass function. The observed core radius-age relation for the LMC clusters favors an intial mass function with slope slightly flatter than the Salpeter value.

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