Cococubed.com Colliding White Dwarfs

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2023 MESA Marketplace
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2022 Earendel, A Highly Magnified Star
2022 White Dwarfs & 12C(α,γ)16O
2022 Black Hole Mass Spectrum
2022 MESA in Don't Look Up
2021 Bill Paxton, Tinsley Prize

Contact: F.X.Timmes
my one page vitae,
full vitae,
research statement, and
teaching statement.
Zero Impact Parameter White Dwarf Collisions in FLASH (collisions III, 2012)
In this article We systematically explore zero impact parameter collisions of white dwarfs (WDs) with the Eulerian adaptive grid code FLASH for 0.64 + 0.64 M$_{\odot}$ and 0.81 + 0.81 MM$_{\odot}$ mass pairings. Our models span a range of effective linear spatial resolutions from 5.2 $\times$ 10$^7$ to 1.2 $\times$ 10$^7$ cm. However, even the highest resolution models do not quite achieve strict numerical convergence, due to the challenge of properly resolving small-scale burning and energy transport. The lack of strict numerical convergence from these idealized configurations suggests that quantitative predictions of the ejected elemental abundances that are generated by binary WD collision and merger simulations should be viewed with caution.

Nevertheless, the convergence trends do allow some patterns to be discerned. We find that the 0.64 + 0.64 M$_{\odot}$ head-on collision model produces 0.32 M$_{\odot}$ of $^{56}$Ni and 0.38 M$_{\odot}$ of $^{28}$Si, while the 0.81 + 0.81 M$_{\odot}$ head-on collision model produces 0.39 M$_{\odot}$ of $^{56}$Ni and 0.55 M$_{\odot}$ of $^{28}$Si at the highest spatial resolutions. Both mass pairings produce $\simeq$ 0.2 M$_{\odot}$ of unburned $^{12}$C+$^{16}$O. We also find the 0.64 + 0.64 M$_{\odot}$ head-on collision begins carbon burning in the central region of the stalled shock between the two WDs, while the more energetic 0.81 + 0.81 M$_{\odot}$ head-on collision raises the initial post-shock temperature enough to burn the entire stalled shock region to nuclear statistical equilibrium.

56Ni Production in Double-degenerate White Dwarf Collisions (collisions II, 2010)
In this article we present a comprehensive study of white dwarf collisions as an avenue for creating type Ia supernovae. Using a smooth particle hydrodynamics code with a 13-isotope, $\alpha$-chain nuclear network, we examine the resulting $^{56}$Ni yield as a function of total mass, mass ratio, and impact parameter. We show that several combinations of white dwarf masses and impact parameters are able to produce sufficient quantities of $^{56}$Ni to be observable at cosmological distances.

We find that the $^{56}$Ni production in double-degenerate white dwarf collisions ranges from sub-luminous to the super-luminous, depending on the parameters of the collision. For all mass pairs, collisions with small impact parameters have the highest likelihood of detonating, but $^{56}$Ni production is insensitive to this parameter in high-mass combinations, which significantly increases their likelihood of detection. We also find that the $^{56}$Ni dependence on total mass and mass ratio is not linear, with larger-mass primaries producing disproportionately more $^{56}$Ni than their lower-mass secondary counterparts, and symmetric pairs of masses producing more $^{56}$Ni than asymmetric pairs.

On Type Ia supernovae from the collisions of two white dwarfs (collisions I, 2009)
In this letter we explore collisions between two white dwarfs as a pathway for making Type Ia supernovae (SNIa). White dwarf number densities in globular clusters allow 10-100, redshift z $\lesssim$ 1 collisions per year, and observations by Chomiuk et al. of globular clusters in the nearby S0 galaxy NGC 7457 have detected what is likely to be a SNIa remnant. We carry out simulations of the collision between two 0.6 M$_{\odot}$ white dwarfs at various impact parameters and mass resolutions. For impact parameters less than half the radius of the white dwarf, we find such collisions produce $\simeq$ 0.4 M$_{\odot}$ of $^{56}$Ni, making such events potential candidates for underluminous SNIa or a new class of transients between Novae and SNIa.