Mathematics – Logic
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt........12b&link_type=abstract
Thesis (PH.D.)--THE OHIO STATE UNIVERSITY, 1995.Source: Dissertation Abstracts International, Volume: 56-06, Section: B, page: 3
Mathematics
Logic
1
Star Formation, Large Magellanic Cloud
Scientific paper
Near infrared (1.25 μm -2.2 μm) imaging and spectroscopy are used to investigate the massive stellar population at the Galactic center and the mass distribution in the inner Galaxy. Radial velocities are presented for approximately 40 stars in each of four optically obscured, off-axis fields toward the Galactic bulge at projected radii between 150 pc and 300 pc from the Galactic center. These velocities are used to compute mean radial velocities and radial velocity dispersions along an axis which is 55^circ from the major axis of the Galaxy. A simple dynamical model of the Galactic bulge is developed using the tensor virial theorem. The model is based, in part, on the mean kinematics described above and new photometric surface brightness modeling from the literature. The model, which considers the bulge as a rotating bar, suggests that it may be considerably more massive than previously thought with a total mass up to 2.8 times 10^{10 } M_odot. R (equivlambda/Delta lambda) ~ 570 resolution K band (2.2mum) spectra are also presented for the He I emission-line sources at the Galactic center (GC); an H band (1.65mum) spectrum is also presented for the most prominent He I star, the AF star. These are compared to similar spectra for nine galactic and Large Magellanic Cloud (LMC) early type mass losing stars, including Ofpe/WN9, WN, and LBV stars. While the GC and comparison star spectra show some morphological similarities, larger He I equivalent widths are found in the AF source and two galactic early type mass losing stars than in any of the LMC stars. Several of the GC He I sources are found to have higher He I velocity widths than any of the galactic or LMC early type mass losing stars. The GC He I sources are not likely to be normal OB giant/supergiants, WC, or WN7-8 stars based on a comparison of the present work to published spectra of these types. The value of the bolometric correction, BC_ {K} = Mbol -MK, is estimated for the GC sources as a function of effective temperature from published data on LBV, WN9, and Ofpe/WN9 stars, and combined with limits on the effective temperature to place the GC sources in the Hertzsprung-Russell diagram. The investigation of the GC massive stellar population includes the discovery of a Wolf-Rayet star located at 0.5 pc projected radius from the center of the Galaxy. This is the first such object to be discovered near the GC; its discovery has strong implications for the character and extent of recent star formation in the region.
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