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- Q2564410 subject Q6441178.
- Q2564410 subject Q6864552.
- Q2564410 subject Q7061010.
- Q2564410 subject Q7217183.
- Q2564410 abstract "Carbon detonation is the violent reignition of thermonuclear fusion in a white dwarf, which produces a Type Ia supernova. A white dwarf undergoes carbon detonation only if it has a normal binary star companion close enough for the dwarf star to siphon sufficient amounts of matter onto itself, the siphoned matter having been expelled during the process of the companion's own late stage stellar evolution.If the companion supplies enough matter to the dead star, the white dwarf's internal pressure and temperature will rise high enough to fuse the previously unfusable carbon in the white dwarf's core. Carbon detonation generally occurs when the accreted matter pushes the white dwarf's mass close to the Chandrasekhar limit of roughly 1.4 solar masses.While heat is released by the fusion reactions, pressure initially is due almost entirely to electron degeneracy pressure rather than thermal energy and thus does not increase much, inhibiting expansion of the star (until too late) and allowing temperature and thus the rate of fusion to increase dramatically in a runaway process. The resumption of fusion spreads outward in a series of uneven, expanding "bubbles" exhibiting Rayleigh–Taylor instability. Within the fusion area, the increase in heat with unchanged volume results in an exponentially rapid increase in the rate of fusion – a sort of supercritical event as thermal pressure increases boundlessly. With no hydrostatic equilibrium possible, this triggers a "thermonuclear flame," and an explosive eruption through the dwarf star's surface that completely disrupts it, seen as a Ia supernova.This process, of a volume supported by electron degeneracy pressure instead of thermal pressure gradually reaching conditions capable of igniting runaway fusion, is also found in a less dramatic form in a helium flash in the core of a sufficiently massive red giant star.".
- Q2564410 wikiPageExternalLink truran-3-1.pdf.
- Q2564410 wikiPageExternalLink hl2004-10-en.html.
- Q2564410 wikiPageWikiLink Q1075685.
- Q2564410 wikiPageWikiLink Q13082.
- Q2564410 wikiPageWikiLink Q180892.
- Q2564410 wikiPageWikiLink Q208470.
- Q2564410 wikiPageWikiLink Q208641.
- Q2564410 wikiPageWikiLink Q3937.
- Q2564410 wikiPageWikiLink Q50053.
- Q2564410 wikiPageWikiLink Q50081.
- Q2564410 wikiPageWikiLink Q51366.
- Q2564410 wikiPageWikiLink Q582000.
- Q2564410 wikiPageWikiLink Q5871.
- Q2564410 wikiPageWikiLink Q623.
- Q2564410 wikiPageWikiLink Q6441178.
- Q2564410 wikiPageWikiLink Q6472.
- Q2564410 wikiPageWikiLink Q6864552.
- Q2564410 wikiPageWikiLink Q7061010.
- Q2564410 wikiPageWikiLink Q7217183.
- Q2564410 wikiPageWikiLink Q865098.
- Q2564410 wikiPageWikiLink Q899055.
- Q2564410 wikiPageWikiLink Q904993.
- Q2564410 wikiPageWikiLink Q908282.
- Q2564410 comment "Carbon detonation is the violent reignition of thermonuclear fusion in a white dwarf, which produces a Type Ia supernova.".
- Q2564410 label "Carbon detonation".