Astronomy research
  Software Infrastructure:
     My codes
  White dwarf supernova:
     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
     Compact object IMF
     Pre-SN variations
     MC white dwarfs
     Classical novae
     He shell convection
     Presolar grains
     He burn on neutron stars
     BBFH at 40 years
  Chemical Evolution:
     Hypatia catalog
     Zone models H to Zn
     Mixing ejecta
     γ-rays within 100 Mpc
  Thermodynamics & Networks
     Stellar EOS
     Reaction networks
     Proton-rich NSE
     MC reaction rates
  Verification Problems:
     Validating an astro code
Software instruments
Bicycle adventures

AAS Journals
2017 MESA Summer School
Teaching materials
Education and Public Outreach
2016 NSF SI2 PI Workshop

Contact: F.X.Timmes
my one page vitae,
full vitae,
research statement, and
teaching statement.
FLASH: An Adaptive Mesh Hydrodynamics Code for Modeling Astrophysical Thermonuclear Flashes (2000)

In this paper, we report on the completion of the first version of a new-generation simulation code, FLASH. The FLASH code solves the fully compressible, reactive hydrodynamic equations and allows for the use of adaptive mesh refinement. It also contains state-of-the-art modules for the equations of state and thermonuclear reaction networks. The FLASH code was developed to study the problems of nuclear flashes on the surfaces of neutron stars and white dwarfs, as well as in the interior of white dwarfs. We expect, however, that the FLASH code will be useful for solving a wide variety of other problems. This first version of the code has been subjected to a large variety of test cases and is currently being used for production simulations of X-ray bursts, Rayleigh-Taylor and Richtmyer-Meshkov instabilities, and thermonuclear flame fronts. The FLASH code is portable and already runs on a wide variety of massively parallel machines, including some of the largest machines now extant.

Riemann problem
Module relationships
Emery wind tunnel

The first bare-knuckles version of FLASH was created by Kevin Olson (he had PARAMESH and his hands on the keyboard), Bruce Fryxell (he had the hydro), and me (had the local physics) in late 1998 in the Laboratory for Astrophysics and Space Research (LASR) building where Kevin and I shared an office. We had some nifty SGI O2 desktop computers at the time. Shortly thereafter Paul Ricker (had the gravity) and Mike Zingale (had the viz and all-purpose skills) added critical capabilities. Jonathan Dursi and Alan Calder made key contributions and gave the development team a critical mass.