Abstract
Wind mass-loss solutions and theoretical light curves for rapid outbursts of recurrent novae are presented for a wide range of parameters of white-dwarf masses of 1.2, 1.3, 1.35, and 1.377 M(fisheye) with envelope compositions of X = 0.7, 0.35, and 0.1 and heavy element contents of Z = 0.001, 0.004, 0.01, 0.02, 0.05, and 0.1. Very rapid optical decline (t3 < 10 days) is obtained only in very massive white dwarfs ( > 1.35 M(fisheye)) for Z = 0.02. Systematic differences of evolutionary time-scale and of the wind velocity are predicted between novae of Populations I and II. The light-curve fittings of four recurrent novae U Sco, V394 CrA, T CrB, and V745 Sco, show that these systems contain a very massive white dwarf of mass 1.35-1.38 M(fisheye).
| Original language | English |
|---|---|
| Pages (from-to) | 525-535 |
| Number of pages | 11 |
| Journal | Publications of the Astronomical Society of Japan |
| Volume | 51 |
| Issue number | 4 |
| DOIs | |
| Publication status | Published - 1999 |
| Externally published | Yes |
Keywords
- Stars: Novae
- Stars: Population II
- Stars: individual (U Scorpii, V394 Coronae Australis, T coronae Borealis, V745 Scorpii)
- Stars: mass loss
- Stars: white dwarfs
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science