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Saturday, July 18, 2020 | History

2 edition of thermonuclear runaway on the surface of a white dwarf found in the catalog.

thermonuclear runaway on the surface of a white dwarf

Marina Orio

thermonuclear runaway on the surface of a white dwarf

by Marina Orio

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  • 10 Currently reading

Published by Max-Planck Institut für Astrophysik in Munich .
Written in English


Edition Notes

Thesis (Ph.D.)--Technion-Israel Institute of Technology.

StatementMarina Orio.
SeriesMPA -- 335, MPA (Series) (Garching bei München, Germany) -- 335
ID Numbers
Open LibraryOL14507318M

Nova eruptions are caused by the buildup of gas on the surface of the white dwarf: eventually, the mass, pressure, and temperature build up and the gas detonates, in a thermonuclear runaway. Nova-like variables do not have eruptions or outbursts, but do have spectra that resemble those of classical novae many years after an eruption. A nova is a thermonuclear detonation on the surface of a white dwarf, and can recur multiple times, as it’s just a surface explosion. This kind of behavior makes these binaries fairly noticeable, because the brightness of the star will flare to many times its original brightness.

  "Eventually enough gas collects on the white dwarf for thermonuclear reactions to begin, similar to those which power the Sun but which runaway into a massive explosion. Microsoft Surface Book.   A white dwarf has no fuel to create any thermonuclear reactions. That was all 'burned' up back when it was a star. A white dwarf has already collapsed. It was once a much bigger star. The gravy collapses it as much as it can, though eventually a balance .

  The resulting thermonuclear explosion hurls off that extra star-stuff from the white dwarf’s surface, creating a nova that can, briefly, be up to a million times brighter than usual. It is clear that the white dwarf has undergone a runaway sometime in the past, the first such evidence of a TNR in a dwarf nova. A TNR on a slowly accreting M white dwarf should produce a classical nova explosion. This is also the first direct evidence of proton capture-processed material in the atmosphere of .


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Thermonuclear runaway on the surface of a white dwarf by Marina Orio Download PDF EPUB FB2

The result was that a thermonuclear runaway on the surface of a white dwarf did not produce the required 10 45 erg of energy observed in the outburst. In retrospect, this result was not surprising given that the mass assumed in the model was much lower than the best estimate at the time for the mass of the white dwarf in DQ Her.

Carbon detonation or Carbon deflagration is the violent reignition of thermonuclear fusion in a white dwarf star that was previously slowly cooling. It involves a runaway thermonuclear process which spreads through the white dwarf in a matter of seconds, producing a Type Ia supernova which releases an immense amount of energy as the star is blown apart.

The carbon detonation/deflagration. A nova results from runaway hydrogen fusion (via the CNO cycle) in the outer layer of a carbon-oxygen white dwarf star. If a white dwarf has a companion star from which it can accrete gas, the material will accumulate in a surface layer made degenerate by the dwarf's intense gravity.

Under the right conditions, a sufficiently thick layer of. Kercek A, Hillebrandt W, Truran JW () Two-dimensional simulations of the thermonuclear runaway in an accreted atmosphere of a C+O white dwarf.

A&A – arXiv:astro-ph/ Google Scholar. A leading model for Type Ia supernovae (SNe Ia) begins with a white dwarf near the Chandrasekhar mass that ignites a degenerate thermonuclear runaway close to its center and explodes.

This second type of supernova is distinct from a surface thermonuclear explosion on a white dwarf, which is called a nova. In either type of supernova, the resulting explosion expels much or all.

Evidence of a Thermonuclear Runaway and Proton-Capture Material on a White Dwarf in a Dwarf Nova Article (PDF Available) in The Astrophysical Journal (1):L17 January with 24 Reads. The most important is that in a classical nova, the thermonuclear runaway occurs only on the surface of the star, allowing the white dwarf and the binary system to remain intact.

In a Type Ia supernova, the thermonuclear runaway occurs within white dwarf itself, completely disrupting the progenitor. Kercek A., Hillebrandt W., Truran J.W. () Two- and three-dimensional simulations of the thermonuclear runaway in an accreted atmosphere of a C+O white dwarf.

In: Bruneau CH. (eds) Sixteenth International Conference on Numerical Methods in Fluid Dynamics. Lecture Notes in Physics, vol Springer, Berlin, Heidelberg.

First Online 02 May Cited by: 5. On 20 Marcha star in the constellation Carina suddenly flared into a nova as gas from a companion sun fell onto the surface of a white dwarf, triggering a runaway thermonuclear explosion that blew off the accumulated material in a titanic outburst.

The All-Sky Automated Survey for Supernovae detected the explosion, one of a wave of flares. Spectral observations obtained soon after the brightening of U Sco support a thermonuclear runaway model for outbursts of this object. Spectra later in the decline are, however, more characteristic of a hot accretion disc.

These observations are reconciled in a model where the low-mass high-velocity shell ejected from the surface of the white dwarf collides with the accretion disc causing Author: K. Sekiguchi, M.W. Feast, P.A. Whitelock, M.D.

Overbeek, W. Wargau, J. Spencer Jones. The white dwarf star slowly accumulates a layer of hydrogen on its surface (see a beautiful simulation of this process by John Blondin).

When about 10 -8 solar masses of hydrogen has been accumulated, the temperature and pressure at the base of this layer will be great enough so that thermonuclear reactions begin (just like in a stellar core).

Abstract: Type Ia Supernovae are thought to be thermonuclear explosions of massive white dwarfs (WD). We present the first study of multi-dimensional effects during the final hours prior to the thermonuclear runaway which leads to the explosion. The calculations utilize an implicit, 2-D hydro and the ignition process are studied in Cited by: C) the complete disintegration of a massive star due to a runaway thermonuclear explosion in the star's interior.

D) matter from a companion star falling onto a white dwarf in a close binary system, eventually causing a nuclear explosion on the dwarf's surface. powered by a thermonuclear runaway in the material accreted onto the surface of a white dwarf star from a close binary companion.

At the peak of their eruptions novae become among the most powerful of celestial sources, with luminosities up to a million times that of the Sun.

It was recognized early on that the peak luminosities of novae were. on the effect of explosive thermonuclear burning on the accreted envelopes of white dwarfs in cataclysmic variables. occurs when a white dwarf accumulates matter from a companion star and steadily increases its mass until a critical density is reached at (or near) its center, triggering a thermonuclear runaway that completely incinerates the star.

Such supersoft sources are associated with a runaway thermonuclear explosion on the surface of the white dwarf.

They usually occur over a relatively short period of time. A nova is created when additional material is accreted onto the hot surface of a white dwarf. If sufficient material is accreted that pushes the mass of the white dwarf over the Chandrasekhar. This higher mass makes for a higher surface gravity, which allows a relatively small amount of matter to reach the ignition point for a thermonuclear runaway.

White dwarfs in. @article{osti_, title = {OPTICAL THERMONUCLEAR TRANSIENTS FROM TIDAL COMPRESSION OF WHITE DWARFS AS TRACERS OF THE LOW END OF THE MASSIVE BLACK HOLE MASS FUNCTION}, author = {MacLeod, Morgan and Ramirez-Ruiz, Enrico and Guillochon, James and Kasen, Daniel and Rosswog, Stephan}, abstractNote = {In this paper, we model the observable .About every 20 years, enough material from the red giant builds up on the surface of the white dwarf to produce a thermonuclear explosion.

The white dwarf orbits close to the red giant, with an accretion disc concentrating the overflowing atmosphere of the red giant onto the white dwarf.Such supersoft sources are associated with a runaway thermonuclear explosion on the surface of the white dwarf.

They usually occur over a relatively short period of time.