Nucleosynthesis in SNIa

Bravo, Eduardo; Isern, J.; Canal, R.; Labay, J.

doi:10.1007/bf00640679

Cited by 42 publications

(60 citation statements)

References 7 publications

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“…As for the fainter peak -expected to be the real age indicator-the age obtained from standard WD models is in conflict (∼ 2 Gyr younger) with that derived from the cluster main-sequence (MS) turn-off (TO), and the age later obtained from the cluster eclipsing binaries studied by Brogaard et al (2012). This discrepancy has led to a detailed reevaluation of the effect of diffusion of 22 Ne in the CO core before crystallization sets in (e.g., Bravo et al 1992, Deloye & Bildsten 2002. As shown by García-Berro et al (2010 with full evolutionary calculations, at the old age and high metallicity of this cluster (about twice solar), the extra-energy contributed by Ne-diffusion in the liquid phase slows down substantially the cooling of the models and can bring into agreement WD, TO and eclipsing binary ages.…”

Section: Introductionmentioning

confidence: 99%

Hubble Space Telescope observations of the Kepler-field cluster NGC 6819 – I. The bottom of the white dwarf cooling sequence★

Bedin

Salaris

Anderson

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We use Hubble Space Telescope (HST ) to reach the end of the white dwarf (WD) cooling sequence (CS) in the solar-metallicity open cluster NGC 6819. Our photometry and completeness tests show a sharp drop in the number of WDs along the CS at magnitudes fainter than m F606W = 26.050 ± 0.075. This implies an age of 2.25 ± 0.20 Gyr, consistent with the age of 2.25 ± 0.30 Gyr obtained from fits to the main-sequence turn-off. The use of different WD cooling models and initial-final-mass relations have a minor impact the WD age estimate, at the level of ∼0.1 Gyr. As an important by-product of this investigation we also release, in electronic format, both the catalogue of all the detected sources and the atlases of the region (in two filters). Indeed, this patch of sky studied by HST (of size ∼70 arcmin 2 ) is entirely within the main Kepler-mission field, so the high-resolution images and deep catalogues will be particularly useful.

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Section: Introductionmentioning

confidence: 99%

Hubble Space Telescope observations of the Kepler-field cluster NGC 6819 – I. The bottom of the white dwarf cooling sequence★

Bedin

Salaris

Anderson

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…If this is the case, the production factor of neutron-rich isotopes with respect to the solar value would be $1.5, which can be increased up to $3 if all the possible uncertainties are taken into account. Previous parameterized studies show that in order to fit this constraint, the ignition density in SNe Ia models has to be 2 ; 10 9 g cm À3 since, otherwise, the neutronized species synthesized during the explosion would be too abundant in the ejected matter (Bravo et al 1993;Höflich & Khokhlov 1996;Woosley 1997;Iwamoto et al 1999;Brachwitz et al 2000Brachwitz et al , 2001. In our models with ig !…”

Section: Formation Of a Remnantmentioning

confidence: 90%

Rotating Type Ia SN Progenitors: Explosion and Light Curves

Domínguez

Piersanti

Bravo

et al. 2006

ApJ

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Based on the rigidly rotating progenitor models found to be able to grow up to the canonical Chandrasekhar mass limit and beyond, and undergo a thermonuclear explosion, we compute the explosions, detailed nucleosynthesis, and corresponding light curves by means of a one-dimensional hydrodynamic code. Our results show that the inclusion of rotation in the evolution of the progenitors determines, in a natural way, a variation in the explosive physical conditions, mainly different explosive ignition densities (2:08 ; 10 9 to 3:34 ; 10 9 g cm À3 ), total masses (1.39-1.48 M ), and binding energies (À5:3 ; 10 50 to À6:6 ; 10 50 ergs). Such a spread is related to the rotational velocity at the explosive carbon ignition stage and to the efficiency of angular momentum loss during the last part of the progenitor evolution. We explore the final outcome in the framework of the delayed detonation explosion models by fixing the value of the transition density and by considering two different braking efficiencies. Within the explored parameter space, the bolometric light curves at maximum show differences of $0.1 mag due to the different amount of 56 Ni synthesized during the explosion. Although rigid rotation cannot be considered responsible for the diversities in the observational properties of SNe Ia, it could explain the dispersion in the magnitude at maximum of standardized events. We also find that those models with high ignition densities produce a central remnant in which most of the neutron-rich species synthesized during the explosion are trapped.

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“…In summary, there is a general consensus about the fact that, in order to explain spectroscopic observations, burning should proceed subsonically (deflagration) in the inner core (where densities are large, i.e., ρ > 10 8 g cm −3 ), whereas burning becomes supersonic (detonation) in the outer lower density zones (see examples of models in Bravo et al 1993, Höflich and Khokhlov 1996, Bravo et al 1996, Woosley 1997. But the way in which the deflagration to detonation transition (DDT) occurs is not yet clear, (see, e.g., discussions in recent papers by Niemeyer and Woosley 1997, Niemeyer 1999, Lisewski, Hillebrandt and Woosley 2000, and in the review by Hillebrandt and Niemeyer 2000).…”

Section: Thermonuclear Supernovae (Sneia)mentioning

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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Nucleosynthesis in SNIa

Cited by 42 publications

References 7 publications

Hubble Space Telescope observations of the Kepler-field cluster NGC 6819 – I. The bottom of the white dwarf cooling sequence★

Hubble Space Telescope observations of the Kepler-field cluster NGC 6819 – I. The bottom of the white dwarf cooling sequence★

Rotating Type Ia SN Progenitors: Explosion and Light Curves

Explosive Nucleosynthesis

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