Convective hydrogen burning down a nova outburst

Glasner, S. Ami; Livne, Eli

doi:10.1086/187911

Cited by 58 publications

(56 citation statements)

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“…the thermonuclear runaway can lead to an enrichment of the accreted envelope with material from the underlying white dwarf at levels that approximately agree with observations (Glasner & Livne 1995;Casanova et al 2011Casanova et al , 2016Glasner et al 2012).…”

Section: Mixing Between White Dwarf and Accreted Matter During The Flashsupporting

confidence: 74%

On Presolar Stardust Grains from CO Classical Novae

Iliadis

Downen²,

José

et al. 2018

ApJ

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About 30%-40% of classical novae produce dust 20-100 days after the outburst, but no presolar stardust grains from classical novae have been unambiguously identified yet. Although several studies claimed a nova paternity for certain grains, the measured and simulated isotopic ratios could only be reconciled, assuming that the grains condensed after the nova ejecta mixed with a much larger amount of close-to-solar matter. However, the source and mechanism of this potential post-explosion dilution of the ejecta remains a mystery. A major problem with previous studies is the small number of simulations performed and the implied poor exploration of the large nova parameter space. We report the results of a different strategy, based on a Monte Carlo technique, that involves the random sampling over the most important nova model parameters: the white dwarf composition; the mixing of the outer white dwarf layers with the accreted material before the explosion; the peak temperature and density; the explosion timescales; and the possible dilution of the ejecta after the outburst. We discuss and take into account the systematic uncertainties for both the presolar grain measurements and the simulation results. Only those simulations that are consistent with all measured isotopic ratios of a given grain are accepted for further analysis. We also present the numerical results of the model parameters. We identify 18 presolar grains with measured isotopic signatures consistent with a CO nova origin, without assuming any dilution of the ejecta. Among these, the grains G270_2, M11-334-2, G278, M11-347-4, M11-151-4, and Ag2_6 have the highest probability of a CO nova paternity.

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Section: Mixing Between White Dwarf and Accreted Matter During The Flashsupporting

confidence: 74%

On Presolar Stardust Grains from CO Classical Novae

Iliadis

Downen²,

José

et al. 2018

ApJ

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“…He suggested that heat transport was too inefficient to spread a localized TNR to the entire surface, concluding that localized, volcanic-like TNRs were likely to occur. The first studies that addressed this question in the framework of multidimensional nova simulations were performed by Glasner et al [32,33]: 2D simulations were performed with the code VULCAN, an arbitrary Lagrangian Eulerian (ALE) code with capability to handle both explicit and implicit steps. Only a slice of the star (i.e., 0.1 π rad), in spherical-polar coordinates with reflecting boundary conditions, was adopted.…”

Section: Multidimensional Modelsmentioning

confidence: 99%

Nucleosynthesis in Novae

José

2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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Remarkable progress in our understanding of nova outbursts has been achieved through combined efforts in photometry, spectroscopy and numerical simulations. According to the thermonuclear runaway model, novae are powered by thermonuclear explosions in the H-rich envelopes transferred from a low-mass stellar companion onto a close white dwarf star. Extensive numerical simulations have shown that the accreted envelopes attain peak temperatures ranging between 100 and 400 MK, for about several hundred seconds, hence allowing extensive nuclear processing which eventually shows up in the form of nucleosynthetic fingerprints in the ejecta. Indeed, it has been claimed that novae can play a key role in the enrichment of the interstellar medium through a number of Al. At the turn of the XXI Century, classical novae entered the era of multidimensional models, which provide new insights into the physical mechanisms that drive mixing at the core-envelope interface. In this paper, we will present an overview on classical nova models, from the onset of accretion up to the explosion and ejection stages, with special emphasis on their gross observational properties and their associated nucleosynthesis. The impact of nuclear uncertainties on the final yields will be discussed.

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“…As such, multidimensional hydrodynamic simulations (see e.g., Refs. [4,[12][13][14][15][16][17]) should be used for improved nucleosynthesis predictions when sufficient computational power is available to model all relevant details of the explosion. To date, multidimensional models have only followed the evolution of a nova over only a very small fraction of the overall time associated with the event (e.g., ∼ 1000 s near the peak temperature, to be compared with the duration of the accretion stage ∼ 10 5 yr).…”

Section: Stellar Models and Nucleosynthesismentioning

confidence: 99%

The unreasonable effectiveness of experiments in constraining nova nucleosynthesis

Parikh

2014

EPJ Web of Conferences

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Abstract. Classical nova explosions arise from thermonuclear ignition in the envelopes of accreting white dwarfs in close binary star systems. Detailed observations of novae have stimulated numerous studies in theoretical astrophysics and experimental nuclear physics. These phenomena are unusual in nuclear astrophysics because most of the thermonuclear reaction rates thought to be involved are constrained by experimental measurements. This situation allows for rather precise statements to be made about which measurements are still necessary to improve the nuclear physics input to astrophysical models. We briefly discuss desired measurements in these environments with an emphasis on recent experimental progress made to better determine key rates.

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Convective hydrogen burning down a nova outburst

Cited by 58 publications

References 0 publications

On Presolar Stardust Grains from CO Classical Novae

On Presolar Stardust Grains from CO Classical Novae

Nucleosynthesis in Novae

The unreasonable effectiveness of experiments in constraining nova nucleosynthesis

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