Sub-Chandrasekhar Mass Models for Supernovae

摘要: For carbon-oxygen white dwarfs accreting hydrogen or helium at rates in the range ~(1-10) ? 10?8 M yr?1, a variety of explosive outcomes is possible well before star reaches Chandrasekhar mass. These are surveyed for dwarf masses (0.7-1.1 ?), accretion ((1-7) yr?1), and initial temperatures (0.01 1 L ?). The results particularly sensitive to convection that goes on during last few minutes explosion. Unless this maintains shallow temperature gradient unless density sufficiently high, accreted does not detonate. Below critical ignition density, which we estimate be (5-10) 105?g?cm?3, either novae deflagrations result. hydrodynamics, nucleosynthesis, light curves, spectra representative sample detonating deflagrating models explored. Some can quite faint indeed, powered peak days by decay 48Cr 48V. Only hottest, most massive considered with smallest layers, show reasonable agreement curves common Type Ia supernovae (SNe Ia). other models, especially those involving lighter dwarfs, shell mass exceeds 0.05 56Ni synthesized 0.01 ?. explosions do look like ordinary SNe any frequently observed transient.