Other
Scientific paper
Aug 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apjs...37..459k&link_type=abstract
Astrophysical Journal Supplement Series, vol. 37, Aug. 1978, p. 459-483.
Other
115
Active Galactic Nuclei, H Lines, Quasars, Seyfert Galaxies, Spectrum Analysis, Active Galaxies, Angular Momentum, Balmer Series, H Beta Line, Infrared Spectra, Ion Production Rates, Optical Thickness, Radiative Transfer
Scientific paper
An attempt is made to account for the observational fact that the intensity ratios of the lower Balmer lines seen in emission from QSOs, type 1 Seyfert galaxies, and other related active galaxies are not what would be expected from the conventional picture of lines generated in a recombining hydrogen plasma. Previous observations of emission-line intensities in QSOs and Seyfert galaxies are reviewed. The various processes included in the rate coefficients of the calculations are then described, viz., free-free, bound-free, and bound-bound transitions, radiative transfer, and angular-momentum mixing. The strengths of the various emission lines are calculated by using more accurate values for the transition rates, including excitation and deexcitation simultaneously, and providing for finite rates in optically forbidden transitions. Numerical results are presented for the cases of ground-state collisional excitation, reabsorption of the upper Balmer lines, and collisional deexcitation. The results are applied to construct a model for the emission-line gas in a QSO and to discuss limits on models of Seyfert galaxies.
Krolik Julian H.
McKee Christopher F.
No associations
LandOfFree
Hydrogen emission-line spectra in quasars and active galactic nuclei 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 Hydrogen emission-line spectra in quasars and active galactic nuclei, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Hydrogen emission-line spectra in quasars and active galactic nuclei will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-944000