Dear Kind Reader,
"Massive white dwarfs in binaries are prime candidates for the progenitors of Type Ia supernovae. The observed properties of Type Ia supernovae put very strong constraints on the progenitors, particularly the complete absence of hydrogen and helium in the spectrum just after the explosion and their appearance in old stellar populations such as elliptical galaxies. Models of exploding white dwarfs are, naturally, very uncertain, but it appears likely that a massive white dwarf composed of carbon and oxygen will explode if it accumulates a layer of helium and then exceeds the Chandrasekhar limit. A proposed mechanism for build-up of helium on a massive white dwarf is steady thermonuclear burning of hydrogen due to accretion from a normal star. The observed counterparts to these binaries are the 'super-soft sources' which are identified by the soft X-ray flux emanating from the hot surface of the white dwarf. However, it appears that the majority of Type Ia supernova cannot be due to super-soft sources because the mass transfer rate must remain within a narrow range for a sufficiently long time to build up sufficient helium. At lower accretion rates the hydrogen does not burn steadily, but is ejected in a series of nova explosions. At higher accretion rates the mass transfer is Eddington-limited. It also appears that super-soft sources are not sufficiently long-lived to give supernova explosions in elliptical galaxies (Leibundgut, 2000).
The competing model to super-soft sources has been the double degenerate scenario, in which the companion to the massive white dwarf is a lower mass white dwarf composed mostly of helium. In this scenario, the mass transfer occurs when gravitational radiation drives the two white dwarfs into contact. The difficulty with this model has been the lack of any observed counterparts. This is not surprising given that only 1 in 500 white dwarfs needs to be a progenitor to explain the observed rate of galactic supernovae and far fewer than 500 white dwarfs have been studied in sufficient detail to reveal whether they are potential supernovae."
A careful review of the deflagration of Type Ia supernovae will indicate that in a large number of cases they do not reach the Chandrasekar limit for deflagration to occur. These current arguments are therefore of interest wthin the generalized theory of relativity of Albert Einstein, yet as recentlhy shown by Andrei Linde and others we may access other energetic continnua such as de Sitter space.
Please review the literature in this regard with earnest care or all is lost.
Yours sincerely,
Paul W. Dixon, Ph.D.
Supernova from Experimentation