Computer Science
Scientific paper
Jul 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1776b&link_type=abstract
IUE Proposal ID #MFGEB
Computer Science
Scientific paper
In order to determine the mass function for the most massive sitars in Associations No. 77 and 96 of the Large Magellanic Cloud (LMC), we propose to obtain observations of the hottest (and brightest) stars in these stellar groups. Our previous IUE observations of these associations have allowed us to determine stellar spectral types with better accuracy than can be achieved using optical techniques. Therefore, it was possible to ascertain accurate positions in the H-R diagram. Although we had chosen our program stars to lie at the upper end of the optical color-magnitude diagram, the uv-spectra have shown that they are not on the main-sequence but are evolved objects. Preliminary analysis also reveals that these observations fit the evolutionary tracks for massive stars (e.g. > 10 solar masses). These data have indicated an important anti-correlation between surface temperature and visual magnitude. Thus, it is necessary to observe objects with bluer B-V colors and fainter optical magnitudes in order to detect the hottest stars in these associations. This is also important in ascertaining the correct age for the associations. These same data can be used to investigate the apparent differences in the mass loss rates for stars in these two associations. Many of these stars are in the proper evolutionary stage for mass loss to be important but we have failed to find evidence for this process in the stars in association No. 77. However, stars in association No. 96 do show evidence for mass loss. To better understand the behavior of the stars in these two associations we are asking for continued observations for the following reasons: 1) Observations of fainter stars (fainter in V) with bluer colors (e.g. V ~ 15, B-V ~ -0.3) are required in order to establish whether the anticorrelation between V and T(eff) continues to fainter magnitudes (e.g. are there really 03 stars lurking at V ~ 15.5). The detection (discovery) of these objects is absolutely essential in determining the mass function. 2) Obtaining spectra of more stars in association No. 96 are needed in order to ascertain if mass-loss rates are higher and line-strengths (abundances) are greater when compared with Association NO. 77. 3)These same observations are needed to establish where the main
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