![]() |
|
||||||||
Home Astronomy research Software Infrastructure: MESA FLASH STARLIB MESA-Web starkiller-astro My instruments White dwarf supernova: Remnant metallicities Colliding white dwarfs Merging white dwarfs Ignition conditions Metallicity effects Central density effects Detonation density effects Tracer particle burning Subsonic burning fronts Supersonic burning fronts W7 profiles Massive star supernova: Rotating progenitors 3D evolution 26Al & 60Fe 44Ti, 60Co & 56Ni Yields of radionuclides Effects of 12C +12C SN 1987A light curve Constraints on Ni/Fe ratios An r-process Neutron Stars and Black Holes: Black Hole Mass Gap Compact object IMF Stars: Neutrino HR diagram Pulsating white dwarfs Pop III with JWST Monte Carlo massive stars Neutrinos from pre-SN Pre-SN variations Monte Carlo white dwarfs SAGB stars Classical novae He shell convection Presolar grains He burn on neutron stars BBFH at 40 years Chemical Evolution: Iron Pseudocarbynes Radionuclides in the 2020s Hypatia catalog Zone models H to Zn Mixing ejecta γ-rays within 100 Mpc Thermodynamics & Networks Stellar EOS 12C(α,γ)16O Rate Proton-rich NSE Reaction networks Bayesian reaction rates Verification Problems: Validating an astro code Su-Olson Cog8 Mader RMTV Sedov Noh Software instruments Presentations Illustrations cococubed YouTube Bicycle adventures Public Outreach Education materials 2022 ASU Solar Systems Astronomy 2022 ASU Energy in Everyday Life AAS Journals AAS YouTube 2022 Earendel, A Highly Magnified Star 2022 TV Columbae, Micronova 2022 White Dwarfs and 12C(α,γ)16O 2022 MESA in Don't Look Up 2022 MESA Marketplace 2022 MESA Summer School 2022 MESA Classroom 2021 Bill Paxton, Tinsley Prize Contact: F.X.Timmes my one page vitae, full vitae, research statement, and teaching statement. |
Spectra of Type Ia Supernovae from Double Degenerate Mergers (mergers II, 2012)
In this article we combine population synthesis, merger, and explosion models with radiation-hydrodynamics light-curve models to study the implications of such a progenitor scenario on the observed Type Ia supernova population. Our standard model, assuming double-degenerate mergers do produce thermonuclear explosions, produces supernova light curves that are broader than the observed type Ia sample. In addition, we discuss how the shock breakout and spectral features of these double-degenerate progenitors will differ from the canonical bare Chandrasekhar-massed explosion models. We conclude with a discussion of how one might reconcile these differences with current observations.
Remnants of Binary White Dwarf Mergers (mergers I, 2010) In this article we carry out a comprehensive smooth particle hydrodynamics simulation survey of double-degenerate white dwarf binary mergers of varying mass combinations in order to establish correspondence between initial conditions and remnant configurations. We find that all but one of our simulation remnants share general properties such as a cold, degenerate core surrounded by a hot disk, while our least massive pair of stars forms only a hot disk. We also find that some of our simulations with massive white dwarfs exhibit helium detonations on the surface of the primary star before complete disruption of the secondary. However, these helium detonations are insufficiently energetic to ignite carbon, and so do not lead to prompt carbon detonations.
|
||||||||
|
---|