Nucleosynthesis in thermonuclear supernovae

  title={Nucleosynthesis in thermonuclear supernovae},
  author={Ivo R. Seitenzahl and Dean M. Townsley},
  journal={arXiv: Solar and Stellar Astrophysics},
The explosion energy of thermonuclear (Type Ia) supernovae is derived from the difference in nuclear binding energy liberated in the explosive fusion of light 'fuel' nuclei, predominantly carbon and oxygen, into more tightly bound nuclear 'ash' dominated by iron and silicon group elements. The very same explosive thermonuclear fusion event is also one of the major processes contributing to the nucleosynthesis of the heavy elements, in particular the iron-group elements. For example, most of the… Expand

Figures from this paper

Nucleosynthesis in Supernovae
We present the status and open problems of nucleosynthesis in supernova explosions of both types, responsible for the production of the intermediate mass, Fe-group and heavier elements (with theExpand
Modeling subgrid combustion processes in simulations of thermonuclear supernovae
Supernovae of type Ia are thought to arise from the thermonuclear incineration of a carbon-oxygen white dwarf stellar remnant. However, the detailed explosion scenario and stellar evolutionary originExpand
Observational properties of thermonuclear supernovae
The explosive death of a star as a supernova is one of the most dramatic events in the Universe. Supernovae have an outsized impact on many areas of astrophysics: they are major contributors to theExpand
Explosive Nucleosynthesis: What We Learned and What We Still Do Not Understand
This review touches on historical aspects, going back to the early days of nuclear astrophysics, initiated by B\(^2\)FH and Cameron, discusses (i) the required nuclear input from reaction rates andExpand
Making the Heaviest Elements in the Universe: A Review of the Rapid Neutron Capture Process
The production of about half the heavy elements beyond Fe and Ni is assigned the rapid neutron capture process (r process). The full understanding faces two open questions. (a) The nucleosynthesisExpand
Type Ia supernovae from non-accreting progenitors
Type Ia supernovae (SNe Ia) are manifestations of stars deficient of hydrogen and helium disrupting in a thermonuclear runaway. While explosions of carbon-oxygen white dwarfs are thought to accountExpand
Synthesis of radioactive elements in novae and supernovae and their use as a diagnostic tool
Abstract Novae and supernovae play a key role in many fields of Astrophysics and Cosmology. Despite their importance, an accurate description of which objects explode and why and how they explode isExpand
Partly burnt runaway stellar remnants from peculiar thermonuclear supernovae
We report the discovery of three stars that, along with the prototype LP 40−365, form a distinct class of chemically peculiar runaway stars that are the survivors of thermonuclear explosions.Expand
SN Ia Explosions from Hybrid Carbon–Oxygen–Neon White Dwarf Progenitors that Have Mixed during Cooling
The creation of "hybrid" white dwarfs, made of a C-O core within a O-Ne shell has been proposed, and studies indicate that ignition in the C-rich central region makes these viable progenitors forExpand
Prospects of direct detection of $^{48}$V gamma-rays from thermonuclear supernovae
Detection of gamma-rays emitted by radioactive isotopes synthesized in stellar explosions can give important insights into the processes that power transients such as supernovae, as well as providingExpand


Nucleosynthesis in multi-dimensional SN Ia explosions
We present the results of nucleosynthesis calculations based on multi-dimensional (2D and 3D) hydrodynamical simulations of the thermonuclear burning phase in type Ia supernovae (hereafter SN Ia).Expand
Sensitivity study of explosive nucleosynthesis in type Ia supernovae: Modification of individual thermonuclear reaction rates
Background: Type Ia supernovae contribute significantly to the nucleosynthesis of many Fe-group and intermediate-mass elements. However, the robustness of nucleosynthesis obtained via models of thisExpand
Explosive Nucleosynthesis in Carbon Deflagration Models of Type I Supernovae
There is increasing evidence that Type I supernovae (SN I) are the main producers of iron-peak elements in the Galaxy. In addition observations of SN I also indicate the existence of appreciableExpand
Neutron-rich Nucleosynthesis in Carbon Deflagration Supernovae
Accreting carbon-oxygen white dwarfs approaching the Chandrasekhar mass may provide a substantial fraction of Type Ia supernovae. The hydrodynamics of nuclear burning in these models remainsExpand
Nucleosynthesis in thermonuclear supernovae with tracers: convergence and variable mass particles
Nucleosynthetic yield predictions for multidimensional simulations of thermonuclear supernovae generally rely on the tracer particle method to obtain isotopic information of the ejected material forExpand
The effects of variations in nuclear interactions on nucleosynthesis in thermonuclear supernovae
Context. Type Ia supernova explosions are violent stellar events important for their contribution to the cosmic abundance of iron peak elements and for their role as cosmological distance indicators.Expand
p-process nucleosynthesis in postshock supernova envelope environments
Nuclear transformations giving rise to the production of the p-process (bypassed) elements are examined within the framework established by explosive nucleosynthesis studies. The guiding assumptionExpand
For the explosion mechanism of Type Ia supernovae (SNe Ia), different scenarios have been suggested. In these, the propagation of the burning front through the exploding white dwarf (WD) starExpand
Implications of low-energy fusion hindrance on stellar burning and nucleosynthesis
We investigate the consequences of a new phenomenological model prediction of strongly reduced low-energy astrophysical S-factors for carbon and oxygen fusion reactions on stellar burning andExpand
Neutronization During Carbon Simmering In Type Ia Supernova Progenitors
When a Type Ia supernova (SN Ia) progenitor first ignites carbon in its core, it undergoes ${\sim} \,10^{3}-10^{4} \,$yr of convective burning prior to the onset of thermonuclear runaway. This carbonExpand