Abstract
We present a model for steady-state winds of systems with super-Eddington luminosities. These radiatively driven winds are expected to be optically thick and clumpy as they arise from an instability-driven porous atmosphere. The model is then applied to derive the mass loss observed in bright classical novae. The main results are as follows. (i) A general relation between the mass-loss rate and the total luminosity in super-Eddington systems. (ii) A natural explanation of the long-duration super-Eddington outflows that are clearly observed in at least two cases (Novae LMC 1988 #1 and FH Serpentis). (iii) A qualitative agreement between the prediction and observations of the mass loss and temperature evolution. (iv) An agreement between the predicted average integrated mass loss of novae as a function of white dwarf mass and its observations. (v) A natural explanation for the 'transition phase' of novae. (vi) Agreement with η Carinae, which was used to double check the theory: the prediction for the mass shed in the star's great eruption agrees with observations to within the measurement error.
| Original language | American English |
|---|---|
| Pages (from-to) | 126-146 |
| Number of pages | 21 |
| Journal | Monthly Notices of the Royal Astronomical Society |
| Volume | 326 |
| Issue number | 1 |
| DOIs | |
| State | Published - 1 Sep 2001 |
| Externally published | Yes |
Keywords
- Hydrodynamics
- Instabilities
- Novae, cataclysmic variables
- Radiative transfer
- Stars: atmospheres