Predictions of infrared recombination lines in stellar winds of hot stars
Abstract
Infrared recombination lines can provide accurate estimates for the velocity and density structure of stellar winds and thus of mass loss. The authors use a simple stellar wind model, hydrogenic approximations and scaling laws to derive information about recombination lines in the ISO range (1 - 100 μm). They estimate that, for a 40000K star, the boundary-level from above which recombination lines originate is in the range n = 2 - 10 for the most abundant elements. The authors give a simple formula to estimate the population of levels above the boundary-level and use this to produce a table of predictions of fluxes and equivalent widths of recombination lines for H, He, C III-IV, N III-V and O III-V.
- Publication:
-
Infrared Spectroscopy in Astronomy
- Pub Date:
- September 1989
- Bibcode:
- 1989ESASP.290..385S
- Keywords:
-
- Hydrogen Recombinations;
- Infrared Spectra;
- Line Spectra;
- O Stars;
- Stellar Winds;
- Infrared Astronomy;
- Mass Distribution;
- Spectrum Analysis;
- Stellar Models;
- Stellar Spectra;
- Variable Mass Systems;
- Astrophysics;
- Stellar Winds: Models;
- O Stars: Stellar Winds;
- O Stars: Mass Loss;
- O Stars: Infrared Lines