| |
 |
| Paper: |
Recurrent Novae: Progenitors of SN Ia? |
| Volume: |
429, Numerical Modeling of Space Plasma Flows, Astronum-2009 |
| Page: |
173 |
| Authors: |
Walder, R.; Folini, D.; Favre, J. M.; Shore, S. N. |
| Abstract: |
We present 3D hydrodynamical simulations of the separated binary RS
Ophiuchi (RS Oph), a recurrent nova and potential progenitor of a SN
Ia. RS Oph is composed of a red giant (RG) and a white dwarf (WD)
whose mass is close to the Chandrasekhar limit. In an isothermal
scenario, the WD accrets about 10% of a 20 km/s RG wind by a
non-Keplerian accretion disk with strong spiral shocks, and about
2% of a 60 km/s RG wind by what we term a ’turbulent accretion ball’. A
significantly larger impact have the thermodynamics. In an adiabatic
scenario only about 0.7% of the 20 km/s RG wind is accreted. The
rate of change of the system separation due to mass and angular
momentum loss out of the system is negative in all three cases
studied, but is ten times smaller for a fast RG wind (60 km/s) than for
a slow RG wind (20 km/s). The results demonstrate that existing nova
models and observed recurrence times fit well together with 3D wind
accretion and that RS Oph is one of the most promising systems to
become an SN Ia. |
|
|
|
|
|
