Interpreting Emission

Interpreting Emission - , and for specifics of AGN...

Info iconThis preview shows page 1. Sign up to view the full content.

View Full Document Right Arrow Icon
Interpreting Emission-Line Spectra Because various emission lines sample different regimes of temperature, density, and ionization, emission spectra are uniquely powerful probes of conditions around active nuclei. Remember, though, that they do sample conditions around the central engine, which we can study only as it affects the surrounding gas. Important references on emission-line processes are Osterbrock, Astrophysics of Gaseous Nebulae and Active Galactic Nuclei (University Science Books); Spitzer, Physical Processes in the Interstellar Medium (Wiley-Interscience); Aller, Physics of Thermal Gaseous Nebulae
Background image of page 1
This is the end of the preview. Sign up to access the rest of the document.

Unformatted text preview: , and for specifics of AGN applications, Davidson and Netzer 1979 (Rev. Mod. Phys. 51, 715) and Peterson's AGN textbook . Review of the recombination theory in the star-formation lecture will be helpful. Every state of an atom or ion has quantum numbers of importance here as follows: Each ( l,s ) pair has multiplicity g = 2s+1- the number of energy levels with distinct j . For historical reasons, different values of l=0,1,2,3 are denoted in spectroscopic notation by S,P,D,F (strong, principal, diffuse, faint), then G,H,. .. A spectroscopic term (atomic state) is denoted by n g L J ....
View Full Document

This note was uploaded on 11/10/2011 for the course AST AST1002 taught by Professor Emilyhoward during the Fall '10 term at Broward College.

Ask a homework question - tutors are online