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Home Astronomy research Software Infrastructure: MESA FLASH-X STARLIB MESA-Web starkiller-astro My instruments White dwarf pulsations: 12C(α,γ) & overshooting Probe of 12C(α,γ)16O Impact of 22Ne Impact of ν cooling Variable white dwarfs MC reaction rates Micronovae Novae White dwarf supernova: Stable nickel production Remnant metallicities Colliding white dwarfs Merging white dwarfs Ignition conditions Metallicity effects Central density effects Detonation density Tracer particle burning Subsonic burning fronts Supersonic fronts W7 profiles Massive stars: Pop III with HST/JWST Rotating progenitors 3D evolution to collapse MC reaction rates Pre-SN variations Massive star supernova: Yields of radionuclides 26Al & 60Fe 44Ti, 60Co & 56Ni SN 1987A light curve Constraints on Ni/Fe An r-process Effects of 12C +12C Neutron Stars and Black Holes: Black Hole spectrum Mass Gap with LVK Compact object IMF He burn neutron stars Neutrino Emission: Neutrino emission from stars Identifying the Pre-SN Neutrino HR diagram Pre-SN Beta Processes Pre-SN neutrinos Stars: Hypatia catalog SAGB stars Nugrid Yields I He shell convection BBFH at 40 years γ-rays within 100 Mpc Iron Pseudocarbynes Pre-Solar Grains: C-rich presolar grains SiC Type U/C grains Grains from massive stars Placing the Sun SiC Presolar grains Chemical Evolution: Radionuclides in 2020s Zone models H to Zn Mixing ejecta Thermodynamics, Opacities & Networks Radiative Opacity Skye EOS Helm EOS Five EOSs Equations of State 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 AAS Journals 2024 AAS YouTube 2024 AAS Peer Review Workshops 2024 ASU Energy in Everyday Life 2024 MESA Classroom Outreach and Education Materials Other Stuff: Bicycle Adventures Illustrations Presentations Contact: F.X.Timmes my one page vitae, full vitae, research statement, and teaching statement. |
The Su-Olson problem consists of a one-dimensional, half-space, non-equilibrium
Marshak wave. The radiative transfer model is a one-group
diffusion approximation with a finite radiation source boundary
condition, where the radiative and material fields are out of
equilibrium. As the energy density of the radiation field increases,
energy is transfered to the material.
Su & Olson (1996)
found a solution, to quadrature, for the distribution of radiative energy and
material temperature as a function of spacetime. This solution
is useful for verifying time-dependent radiation diffusion codes.
This article,
this article,
and this article,
discuss analytic and numerical solutions for the Su-Olson problem.
The tools in su_olson.tbz reproduce the tables in the Su & Olson article and provide solutions as a function of time and position.
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