Thermonuclear Supernovae

Röpke, F. K.

doi:10.22323/1.060.0024

Cited by 4 publications

(5 citation statements)

References 81 publications

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“…In this section, we will briefly summarize the main characteristics of the different regimes proposed so far. More details can be found in [266,350,351].…”

Section: Ignition Regimesmentioning

confidence: 99%

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Nuclear astrophysics: the unfinished quest for the origin of the elements

José

Iliadis

2011

Rep. Prog. Phys.

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Abstract. Half a century has passed since the foundation of nuclear astrophysics. Since then, this discipline has reached its maturity. Today, nuclear astrophysics constitutes a multidisciplinary crucible of knowledge that combines the achievements in theoretical astrophysics, observational astronomy, cosmochemistry and nuclear physics. New tools and developments have revolutionized our understanding of the origin of the elements: supercomputers have provided astrophysicists with the required computational capabilities to study the evolution of stars in a multidimensional framework; the emergence of high-energy astrophysics with space-borne observatories has opened new windows to observe the Universe, from a novel panchromatic perspective; cosmochemists have isolated tiny pieces of stardust embedded in primitive meteorites, giving clues on the processes operating in stars as well as on the way matter condenses to form solids; and nuclear physicists have measured reactions near stellar energies, through the combined efforts using stable and radioactive ion beam facilities.This review provides comprehensive insight into the nuclear history of the Universe and related topics: starting from the Big Bang, when the ashes from the primordial explosion were transformed to hydrogen, helium, and few trace elements, to the rich variety of nucleosynthesis mechanisms and sites in the Universe. Particular attention is paid to the hydrostatic processes governing the evolution of low-mass stars, red giants and asymptotic giant-branch stars, as well as to the explosive nucleosynthesis occurring in core-collapse and thermonuclear supernovae, γ-ray bursts, classical novae, X-ray bursts, superbursts, and stellar mergers.

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“…In this section, we will briefly summarize the main characteristics of the different regimes proposed so far. More details can be found in [266,350,351].…”

Section: Ignition Regimesmentioning

confidence: 99%

“…Extensive multidimensional simulations are needed to clarify these issues. The interested reader is referred to some of the existing monographs and reviews on type Ia supernovae, for further information [266,350,351,[392][393][394][395].…”

Section: Nucleosynthesis: Type Ia Supernovae As Galactic Fe Factoriesmentioning

confidence: 99%

Nuclear astrophysics: the unfinished quest for the origin of the elements

José

Iliadis

2011

Rep. Prog. Phys.

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“…Pure detonations of Chandrasekhar-mass WDs produce almost no intermediate mass elements (IME) because of the high densities ( 10 7 g cm −3 in most of the WD; Arnett et al 1971, see also introduction in Khokhlov 1991a). Pure deflagrations have recently been identified as promising models for 2002cx-like SNe Ia (Jordan et al 2012b;Kromer et al 2013), but in other parameter ranges they fail to reproduce SNe Ia (Fink et al 2014;Ma et al 2013;Röpke 2008). The densities through which the detonation propagates have to be lowered to produce more IME.…”

Section: Introductionmentioning

confidence: 99%

The white dwarf’s carbon fraction as a secondary parameter of Type Ia supernovae

Ohlmann

Kromer

Fink

et al. 2014

A&A

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Context. Binary stellar evolution calculations predict that Chandrasekhar-mass carbon/oxygen white dwarfs (WDs) show a radially varying profile for the composition with a carbon depleted core. Many recent multi-dimensional simulations of Type Ia supernovae (SNe Ia), however, assume the progenitor WD has a homogeneous chemical composition. Aims. In this work, we explore the impact of different initial carbon profiles of the progenitor WD on the explosion phase and on synthetic observables in the Chandrasekhar-mass delayed detonation model. Spectra and light curves are compared to observations to judge the validity of the model. Methods. The explosion phase is simulated using the finite volume supernova code L, which is extended to treat different compositions of the progenitor WD. The synthetic observables are computed with the Monte Carlo radiative transfer code A. Results. Differences in binding energies of carbon and oxygen lead to a lower nuclear energy release for carbon depleted material; thus, the burning fronts that develop are weaker and the total nuclear energy release is smaller. For otherwise identical conditions, carbon depleted models produce less 56 Ni. Comparing different models with similar 56 Ni yields shows lower kinetic energies in the ejecta for carbon depleted models, but only small differences in velocity distributions and line velocities in spectra. The light curve width-luminosity relation (WLR) obtained for models with differing carbon depletion is roughly perpendicular to the observed WLR, hence the carbon mass fraction is probably only a secondary parameter in the family of SNe Ia.

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“…The final fate of all the scenarios described above, as well as the main characteristics of the ensuing type Ia explosion -whenever it occurs-are tightly related to the details of the burning propagation, which are reviewed by Roepke in this volume [37]. However, it is worth reminding that the presupernova evolution, leading to the initial stages of the ignition, also plays a very important role on the further development of the explosion, whatever the scenario is.…”

Section: Pos(supernova)014mentioning

confidence: 99%

“…There is a complicated interplay between type of accretion and initial white dwarf conditions, such that it is not straightforward to reach the carbon ignition conditions. Once ignition occurs, other problems occur, related to the flame propagation; these are out of the scope of this paper, but are treated in other papers of this volume (e.g., Roepke's contribution [37]). …”

Section: Introductionmentioning

confidence: 99%

Accreting white dwarf

Hernanz¹,

José²

2008

Proceedings of Supernovae: Lights in the Darkness — PoS(SUPERNOVA)

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Thermonuclear (type Ia) supernovae are explosions in accreting white dwarfs, but the exact scenario leading to these explosions is still unclear. An important step to clarify this point is to understand the behaviour of accreting white dwarfs in close binary systems. The characteristics of the white dwarf (mass, chemical composition, luminosity), the accreted material (chemical composition) and those related with the properties of the binary system (mass accretion rate), are crucial for the further evolution towards the explosion. An analysis of the outcome of accretion and the implications for the growth of the white dwarf towards the Chandrasekhar mass and its thermonuclear explosion is presented.

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Thermonuclear Supernovae

Cited by 4 publications

References 81 publications

Nuclear astrophysics: the unfinished quest for the origin of the elements

Nuclear astrophysics: the unfinished quest for the origin of the elements

The white dwarf’s carbon fraction as a secondary parameter of Type Ia supernovae

Accreting white dwarf

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