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Free keywords:
Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,General Relativity and Quantum Cosmology, gr-qc
Abstract:
The thermonuclear explosion of a C/O white dwarf as a Type Ia supernova (SN
Ia) generates a kinetic energy comparable to that released by a massive star
during a SN II event. Current observations and theoretical models have
established that SNe Ia are asymmetric, and therefore -- like SNe II --
potential sources of gravitational wave (GW) radiation. We establish an
upper-bound GW amplitude and expected frequency range based upon the energetics
and nucleosynthetic yields of SNe Ia. We perform the first detailed
calculations of the gravitationally-confined detonation (GCD) mechanism within
the single-degenerate channel of SNe Ia. The GCD mechanism predicts a
strongly-polarized GW burst from the SD channel of SNe Ia in the frequency band
around 1 Hz. Third-generation spaceborne GW observatories currently in
planning, including the Big Bang Observer (BBO), and the Deci-Hertz
Interferometer Gravitational Wave Observatory (DECIGO), as well as earthbound
instruments, including the Einstein Telescope (ET), may be able to detect the
signal predicted by the GCD mechanism from galactic SNe Ia and nearby
extragalactic SNe Ia at distances up to 1 Mpc. If observable, GWs may offer a
direct probe into the first few seconds of SNe Ia, and yield insights into its
underlying detonation mechanism not possible in the optical portion of the
spectrum.
