Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...251..417p&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 251, no. 2, Nov. 1991, p. 417-430. Research supported by CONACYT, FONDECYT, Un
Astronomy and Astrophysics
Astrophysics
30
Abundance, Emission Spectra, H Ii Regions, Interstellar Matter, Line Spectra, Spectrophotometry, Chemical Composition, Ionized Gases, Metallicity, Radial Velocity, Red Shift
Scientific paper
Spectrophotometry of 42 recently discovered southern H II galaxies is presented, and the physical conditions and He, N, Ne, and O abundances of the ionized regions of these galaxies are derived. Most of the objects are found to have a log O/H in the range of 7.9 and 8.3. A close correlation between Ne and O abundances is found. The relationship between some oxygen emission line intensity ratios and the physical conditions of the ionized region is discussed by comparing the observational data with the predictions of a grid of ionization structure models. The behavior of the effective temperature of the ionizing cluster and the ionization parameter for different metallicities are studied. The mean T(eff) of the high O abundance H II galaxies is found to be lower than that in low-abundance objects. The ionization parameter for the regions in the sample is estimated and a mean value of 0.005 is derived. From the galaxies showing the highest ionization degree, it is deduced that, for a given O abundance, there is an upper limit for the ionization parameter, which increases smoothly with decreasing metallicity.
Maza Jose
Peña Manuel
Ruiz María Teresa
No associations
LandOfFree
Line analysis and nebular abundances in H II galaxies does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Line analysis and nebular abundances in H II galaxies, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Line analysis and nebular abundances in H II galaxies will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1716267