81 research outputs found
Recalibration of Pagel's method for HII regions considering the thermal structure, the ionization structure, and the depletion of O into dust grains
Using a sample of 28 HII regions from the literature with measured
temperature inhomogeneity parameter, t^2, we present a statistical correction
to the chemical abundances determined with the Te(4363/5007) method. We used
the t^2 values to correct the oxygen gaseous abundances and consider the oxygen
depletion into dust to calculate the total abundances for these objects. This
correction is used to obtain a new calibration of Pagel's strong-line method,
R_{23}, to determine oxygen abundances in HII regions. Our new calibration
simultaneously considers the temperature structure, the ionization structure,
and the fraction of oxygen depleted into dust grains. Previous calibrations in
the literature have included one or two of these factors; this is the first
time all three are taken into account. This recalibration conciliates the
systematic differences among the temperatures found from different methods. We
find that the total correction due to thermal inhomogeneities and dust
depletion amounts to an increase in the O/H ratio of HII regions by factors of
1.7 to 2.2 (or 0.22 to 0.35 dex). This result has important implications in
various areas of astrophysics such as the study of the higher end of the
initial mass function, the star formation rate, and the mass-metallicity
relation of galaxies, among others.Comment: 16 pages (preprint), 4 figures, 1 Table, accepted in ApJ
HII Regions And the Protosolar Helium, Carbon, and Oxygen Abundances in the Context of Galactic Chemical Evolution
We present chemical evolution models of the Galactic disk with different
Z-dependent yields. We find that a moderate mass loss rate for massive stars of
solar metallicity produces an excellent fit to the observed C/H and C/O
gradients of the Galactic disk. The best model also fits: the H, He, C, and O
abundances derived from recombination lines of M17, the protosolar
abundances,and the C/O-O/H, C/Fe-Fe/H, and O/Fe-Fe/H relations derived from
solar vicinity stars. The agreement of the model with the protosolar abundances
implies that the Sun originated at a galactocentric distance similar to the one
it has. Our model for kpc implies that a fraction of the stars in the
direction of the bulge formed in the inner disc. We obtain a good agreement
between our model and the C/O versus O/H relationship derived from
extragalactic H~{\sc ii} regions in spiral galaxies.Comment: 30 pages, 11 figures. Rev. Mex. Astron. Astrof. accepte
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