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2025 Neutrinos From De-excitation
Radiative Opacity
2024 Neutrino Emission from Stars
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Software Instruments
Stellar equation of states
EOS with ionization
EOS for supernovae
Chemical potentials
Stellar atmospheres
Voigt Function
Jeans escape
Polytropic stars
Cold white dwarfs
Adiabatic white dwarfs
Cold neutron stars
Stellar opacities
Neutrino energy loss rates
Ephemeris routines
Fermi-Dirac functions
Polyhedra volume
Plane - cube intersection
Coating an ellipsoid
Nuclear reaction networks
Nuclear statistical equilibrium
Laminar deflagrations
CJ detonations
ZND detonations
Fitting to conic sections
Unusual linear algebra
Derivatives on uneven grids
Pentadiagonal solver
Quadratics, Cubics, Quartics
Supernova light curves
Exact Riemann solutions
1D PPM hydrodynamics
Hydrodynamic test cases
Galactic chemical evolution
Universal two-body problem
Circular and elliptical 3 body
The pendulum
Phyllotaxis
MESA
MESA-Web
FLASH
Zingale's software
Brown's dStar
GR1D code
Iliadis' STARLIB database
Herwig's NuGRID
Meyer's NetNuc
AAS Journals
2025 AAS YouTube
2025 AAS Peer Review Workshops
2025 ASU Energy in Everyday Life
2025 MESA Classroom
Other Stuff:
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Contact: F.X.Timmes
my one page vitae,
full vitae,
research statement, and
teaching statement.
The tool public_atmos.tbz implements a simple stellar atmosphere model. It assumes a one-dimensional slab in hydrostatic and local thermodynamic equilibrium with gray rosseland mean opacities. Still, it can be useful as a quick diagnostic of a stellar atmosphere, or for checking the effects of a more elaborate piece of local physics (e.g., ionization, such as the figure on the right).
1 M☉ temperature structure |
1 M☉ ionization structure |