Computer Science – Sound
Scientific paper
Nov 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000phdt........68j&link_type=abstract
ProQuest Dissertations And Theses; Thesis (Ph.D.)--The University of Texas at Austin, 2000.; Publication Number: AAT9983244; ISB
Computer Science
Sound
3
Scientific paper
Abundances and kinematics have been determined for sixty-one low metallicity ([Fe/H] < -1.30) stars in an attempt to find correlations between stellar chemistry and dynamics. Distances for program stars have been re-derived spectroscopically, and the computed stellar distances agree with the parallaxes reported by Hipparcos (ESA 1997). Stellar orbits were calculated using the Galactic mass model of Bahcall et al. (1983). We find that the general kinematic results (U, V, W, Rapo, Z max, eccentricity) are more extreme than previously thought, but in good agreement with recent studies of this nature. We have also adopted the chemical and kinematic results for 34 additional stars from the work of others to supplement our sample. Our LTE abundance results concur with previous studies. Specifically, we have found that the alpha-capture elements (Mg, Ca, and Ti) are consistently overabundant by 0.4 dex (i.e. [alpha/Fe] = +0.4) except in the cases of four stars: HD 134439, HD 134440, BD+80 245 and G4-36. Additionally, we have found a typical oxygen overabundance of +0.70 dex, and a sodium abundance of [Na/Fe] = -0.60 dex after an empirical correction for NLTE effects. We find no statistically sound correlations between various kinematic parameters and abundances. We confirm the unusual abundance signatures of HD 134439/HD 134440 and BD+80 245. The former stars are a proper-motion pair with mildly deficient alpha-capture abundances. The latter star possesses a pronounced alpha-capture deficiency combined with an extremely low Ba abundance. Its Na and O are apparently normal. We have also discovered a star with extremely unusual abundances: G4-36 possesses marked deficiencies in O, Mg, Al, Ca, Sr, and Ba, but overabundances of Fe-peak elements Mn, Ni, and Zn. We suggest that the nucleosynthetic origin of G4-36 is substantially different from that of BD+80 245 and the proper motion pair HD 134439/134440. All four unusual stars are in retrograde orbits, as are half the stars in our sample, and all four possess apogalactic distances over 25 kpc, as does about 20% of our entire sample. It is unclear at this point whether the unusual stars are representative of accretion events.
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