Carbon Detonations in Rapidly Rotating White Dwarfs

Details Carbon Detonations in Rapidly Rotating White Dwarfs Carbon Detonations in Rapidly Rotating White Dwarfs

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...254..177s&link_type=abstract

Astronomy and Astrophysics, Vol.254, NO. FEB(I), P. 177, 1992

Astronomy and Astrophysics

Astrophysics

18

Stars: White Dwarfs, Supernovae And Supernovae Remnants: General, Hydrodynamics

Scientific paper

We have performed a set of two-dimensional hydrodynamic simulations of the propagation of detonation waves in rapidly rotating white dwarfs. The axisymmetric initial models used in the simulations are in rotational equilibrium and possess a density stratification similar to that of configurations predicted by the merging scenario of Type Ia supernovae. The energy release is approximated by a single exothermic nuclear reaction 14 12C → 3 56Ni proceeding at the rate of the 12C(12C,4He)20Ne reaction. Central and off-center ignitions have been studied.
When burning is ignited in the center our results show, that independently of the shape of the star, all matter is burned into iron group elements and the star is completely disrupted after typically 200 msec. Igniting the white dwarf in an extended central region having a more or less flattened spheroidal or cylindrical shape gives rise to an initially different behaviour, but within about 100 msec the shape of the detonation wave approaches that of one being ignited only in the center. When burning is ignited off-center all carbon is consumed, too. Thus detonations in non-spherical massive white dwarfs cannot explain the observed intermediate mass elements seen in the spectra of Type Ia supernovae.

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