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 thereforelike 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 and first for a SN Ia of any type 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.
We demonstrate that the integrated gravitational wave signal of Type Ia supernovae (SNe Ia) in the single-degenerate channel out to cosmological distances gives rise to a continuous background to spaceborne gravitational wave detectors, including the Big Bang Observer (BBO) and Deci-Hertz Interferometer Gravitational wave Observatory (DECIGO) planned missions. This gravitational wave background from SNe Ia acts as a noise background in the frequency range 0.1 -10 Hz, which heretofore was thought to be relatively free from astrophysical sources apart from neutron star binaries, and therefore a key window in which to study primordial gravitational waves generated by inflation. While inflationary energy scales of 10 16 GeV yield inflationary gravitational wave backgrounds in excess of our range of predicted backgrounds, for lower energy scales of ∼ 10 15 GeV, the inflationary gravitational wave background becomes comparable to the noise background from SNe Ia.
The discovery of the accelerated expansion of the universe using Type Ia supernovae (SNe Ia) has stimulated a tremendous amount of interest in the use of SNe Type Ia events as standard cosmological candles, and as a probe of the fundamental physics of dark energy. Recent observations of SNe Ia have indicated a significant population difference depending on the host galaxy. These observational findings are consistent with SNe Ia Ni-56 production in star-forming spiral galaxies some 0.1 solar masses higher -and therefore more luminousthan in elliptical galaxies. We present recent full-star, 3D simulations of Type Ia supernovae which may help explain the nature of this systematic variation in SNe Ia luminosities, as well as the nature of the Ia explosion mechanism. These insights may in turn eventually shed light on the mystery of dark energy itself.
scite is a Brooklyn-based organization that helps researchers better discover and understand research articles through Smart Citations–citations that display the context of the citation and describe whether the article provides supporting or contrasting evidence. scite is used by students and researchers from around the world and is funded in part by the National Science Foundation and the National Institute on Drug Abuse of the National Institutes of Health.