Statistics – Computation
Scientific paper
Nov 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...298..660k&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 298, Nov. 15, 1985, p. 660-675. Research supported by the University of Cal
Statistics
Computation
50
Early Stars, Hot Stars, Radiation Pressure, Shock Wave Propagation, Stellar Winds, Computational Astrophysics, Line Spectra, Optical Thickness, Propagation Velocity, Stellar Evolution, Ultraviolet Spectra, X Ray Spectra
Scientific paper
The authors outline the dynamical theory of radiation pressure-driven shocks in winds from early-type stars. After isolating the principal parameters needed for a description of these shocks, namely their speeds relative to incoming material and their column densities, the authors estimate the shocks' principal properties as functions of these parameters. For the special case of time-steady shocks detailed numerical calculations are presented of the shocks' internal structure: density, ionization state, temperature, and flow velocity as functions of position; and X-ray emissivity, UV line emissivity, and total radiation force as functions of shock velocity and postshock column density.
Krolik Julian H.
Raymond John C.
No associations
LandOfFree
Radiation pressure-driven shocks in winds from hot stars 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 Radiation pressure-driven shocks in winds from hot stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Radiation pressure-driven shocks in winds from hot stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-977969