An extended grid of multicycle nova evolution models

Prialnik, Dina; Kovetz, A.

doi:10.1086/175741

Cited by 336 publications

(453 citation statements)

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“…Throughout the calculations, we use a hydrodynamic Lagrangian code, designed to evolve a WD through multiple consecutive nova cycles (Prialnik & Kovetz, 1995). The code simulates the evolution of a WD accreting mass and periodically producing nova outbursts.…”

Section: Model and Calculations Descriptionmentioning

confidence: 99%

Observational signatures of SNIa progenitors, as predicted by models

Hillman

Prialnik

Kovetz

et al. 2014

Monthly Notices of the Royal Astronomical Society

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A definitive determination of the progenitors of type Ia supernovae (SNIa) has been a conundrum for decades. The single degenerate scenario -a white dwarf (WD) in a semi-detached binary system accreting mass from its secondary -is a plausible path; however, no simulation to date has shown that such an outcome is possible. In this study, we allowed a WD with a near Chandrasekhar mass of 1.4M ⊙ to evolve over tens of thousands of nova cycles, accumulating mass secularly while undergoing periodic nova eruptions. We present the mass accretion limits within which a SNIa can possibly occur. The results showed, for each parameter combination within the permitted limits, tens of thousands of virtually identical nova cycles where the accreted mass exceeded the ejected mass, i.e. the WD grew slowly but steadily in mass. Finally, the WD became unstable, the maximal temperature rose by nearly two orders of magnitude, heavy element production was enhanced by orders of magnitude and the nuclear and neutrino luminosities became enormous. We also found that this mechanism leading to WD collapse is robust, with WDs in the range 1.0 -1.38M ⊙ , and an accretion rate of 5 × 10 −7 M ⊙ yr −1 , all growing steadily in mass. These simulations of the onset of a SNIa event make observationally testable predictions about the light curves of pre-SN stars, and about the chemistry of SNIa ejecta.

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Section: Model and Calculations Descriptionmentioning

confidence: 99%

Observational signatures of SNIa progenitors, as predicted by models

Hillman

Prialnik

Kovetz

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…In the case of V838 Mon the outburst appears to have occurred in a binary system, -6 -which may suggest an analogy with a nova system in which a thermonuclear explosion occurs on an accreting white-dwarf companion. However, a broad theoretical exploration 28 of the parameter space for thermonuclear runaways on accreting white dwarfs predicts no behavior like that of V838 Mon. Evidently, V838 Mon has in the recent past had several similar outbursts, which produced the dust envelope that is now being illuminated.…”

Section: V838mentioning

confidence: 99%

An energetic stellar outburst accompanied by circumstellar light echoes

Bond

Henden

Levay

et al. 2003

Nature

224

272

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Some classes of stars, including supernovae and novae, undergo explosive outbursts that eject stellar material into space. In 2002, the previously unknown variable star V838 Monocerotis brightened suddenly by a factor of about 10^4. Unlike a supernova or nova, V838 Mon did not explosively eject its outer layers; rather, it simply expanded to become a cool supergiant with a moderate-velocity stellar wind. Superluminal light echoes were discovered as light from the outburst propagated into surrounding, pre-existing circumstellar dust. Here we report high-resolution imaging and polarimetry of the light echoes, which allow us to set direct geometric distance limits to the object. At a distance of >6 kpc, V838 Mon at its maximum brightness was temporarily the brightest star in the Milky Way. The presence of the circumstellar dust implies that previous eruptions have occurred, and spectra show it to be a binary system. When combined with the high luminosity and unusual outburst behavior, these characteristics indicate that V838 Mon represents a hitherto unknown type of stellar outburst, for which we have no completely satisfactory physical explanation.Comment: To appear in Nature, March 27, 2003. 9 pages, 6 figure

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“…Therefore, it is known that some mixing with core material (either CO or ONe) during the accretion phase prior to the runaway should occur, but this process has not been modeled yet in a self-consistent way. Another approach to the problem of initial enrichment comes from the multicycle 1D models (of CO novae only, up to now), from Prialnik and Kovetz Kovetz 1995, Kovetz andPrialnik, 1997); diffusion is responsible for the enrichment, which becomes larger after a number of flashes. However, the large metallicities and neon abundances observed in some novae are not well reproduced.…”

Section: Classical Novaementioning

confidence: 99%

Explosive Nucleosynthesis

Hernanz¹

2011

Encyclopedia of Astrobiology

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Many radioactive nuclei relevant for gamma-ray astrophysics are synthesized during explosive events, such as classical novae and supernovae. A review of recent results of explosive nucleosynthesis in these scenarios will be presented, with a special emphasis on the ensuing gamma-ray emission from individual nova and supernova explosions. The influence of the dynamic properties of the ejecta on the gamma-ray emission features, as well as the still remaining uncertainties in nova and supernova modelling will also be reviewed.

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An extended grid of multicycle nova evolution models

Cited by 336 publications

References 0 publications

Observational signatures of SNIa progenitors, as predicted by models

Observational signatures of SNIa progenitors, as predicted by models

An energetic stellar outburst accompanied by circumstellar light echoes

Explosive Nucleosynthesis

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