# Astrophysics of Gaseous Nebulae and Active Galactic Nuclei

@inproceedings{Osterbrock1989AstrophysicsOG,
title={Astrophysics of Gaseous Nebulae and Active Galactic Nuclei},
author={Donald E. Osterbrock and Gary J. Ferland},
year={1989}
}
• Published 1989
• Physics
Preface Preface to First Edition General Introduction Photoionization Equilibrium Thermal Equilibrium Calculation of Emitted Spectrum Comparison of Theory with Observations Internal Dynamics of Gaseous Nebulae Interstellar Dust Infrared Radiation and Molecules H II Regions in the Galactic Context Planetary Nebulae Heavy Elements and High-Energy Effects Nova and Supernova Remnants Active Galactic Nuclei Diagnostics and Physics Active Galactic Nuclei Results Appendix 1: Measures of Light Appendix…
5,735 Citations
This chapter presents a review on the latest advances in the computation of physical conditions and chemical abundances of elements present in photoionized gas (H ii regions and planetary nebulae).
Collisions of atoms, ions, electrons and molecules play an important role in the interpretation of astronomical observations and in our understanding of the physical characteristics and the history
The atomic physics relevant to gaseous nebulae is critically examined using modelling software with particular emphasis on radio recombination lines (RRLs). The theoretical spectral line intensities
A wide variety of astrophysical objects, ranging from newly formed stars to accreting black holes, produce ionizing radiation. Nearby material will reprocess these photons into other forms of light.
A combination of photoionization and photodissociation region codes is used to model planetary nebulae and the Crab Nebula supernova remnant, to explain the observed molecular emission. The inclusion
Galactic and extragalactic abundance studies of H II regions, planetary nebulae, and supernova remnants are compiled and their implications briefly reviewed. Galaxy global metallicity appears to be
Here I describe recent studies of objects with molecular hydrogen emission that is strong relative to other spectral lines. Large telescopes and fast spectrometers have made the 2 {\mu}m window
• Physics
• 2017
Accurate rates for energy-degenerate l-changing collisions are needed to determine cosmological abundances and recombination. There are now several competing theories for the treatment of this
• Physics
• 2016
We present a new model of the nebular emission from star-forming galaxies in a wide range of chemical compositions, appropriate to interpret observations of galaxies at all cosmic epochs. The model
• Physics
• 2000
To explain the effects of the ultraviolet (UV) background radiation on the collapse of pre-galactic clouds, we implement a radiation–hydrodynamical calculation, combining one-dimensional spherical