Radiatively-Driven Stellar Winds.
Abstract
An attempt is made to show that the large mass outflows observed in highly luminous stars results from the force of radiation pressure. To calculate this force, it was necessary to compute and/or compile oscillator strengths from ions in the third to sixth stage of ionization of the 21 elements of greatest cosmic abundance. The hydrodynamic equations were solved using this calculated force, and the resultant model agrees with observation to within the accuracy of the calculations. The main properties of the stellar wind are: (1) the rate of mass loss is proportional to the luminosity, and (2) the terminal velocity scales with the photospheric escape velocity, (3) the density structure is of the core/halo type, and (4) the properties of the envelope will be very sensitive to any gradients in the radiation force.
- Publication:
-
Ph.D. Thesis
- Pub Date:
- May 1977
- Bibcode:
- 1977PhDT.........3A
- Keywords:
-
- Physics: Astronomy and Astrophysics;
- Radiation Pressure;
- Stellar Winds;
- Computation;
- Hydrodynamic Equations;
- Ions;
- Luminosity;
- Terminal Velocity;
- Astrophysics