The stellar content of LH 9 and 10 (N11) in the LMC - A case for sequential star formation

Details The stellar content of LH 9 and 10 (N11) in the LMC - A case for sequential star formation The stellar content of LH 9 and 10 (N11) in the LMC - A case for sequential star formation

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aj....103.1205p&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 103, April 1992, p. 1205-1233, 1422-1424.

Astronomy and Astrophysics

Astronomy

143

B Stars, Magellanic Clouds, O Stars, Star Formation, Ubv Spectra, Color-Magnitude Diagram, H Ii Regions, Hertzsprung-Russell Diagram, Interstellar Extinction, Stellar Spectra

Scientific paper

The young OB associations Lucke-Hodge 9 and 10 are studied with UBV photometry that is independent of reddening to determine the IMF directly from star counts. The temperature and reddening of the stars are determined which, in conjunction with the spectroscopic classification of the earliest stars, is employed to place the stellar groups on the theoretical H-R diagram. Observations are also presented of the highly compact H II region/knot N11A and the multiple system HD 32228, and LH 9 and 10 are compared. The Lyman ionizing flux calculated at 4.9-7.2 x 10 exp 50/s agrees well with flux required to generate the H-alpha luminosity of the H II region. LH 10 has a much flatter slope, a higher ratio of higher-mass to lower-mass stars, and greater reddening than LH 9, and LH 10 contains all of the O stars earlier than O6. It is concluded that LH 9 is older than LH 10 and probably contributed to the initiation of star formation in LH 10.

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