Cococubed.com 26Al and 60Fe From Supernovae Explosions
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.	Inner Milky Way Summary (2015): Models: In this article, we explore the current abundances, fluxes, and spatial distributions of two key gamma-ray radioactivities, $^{26}$Al and $^{60}$Fe using recently calculated yields for Type II supernovae, along with models for chemical evolution and the distribution of mass in the interstellar medium. The estimated steady state production rates are 2.0 $\pm$ 1.0 M$_{\odot}$ / Myr for $^{26}$Al and 0.75 $\pm$ M$_{\odot}$ / Myr for $^{60}$Fe. This corresponds to 2.2 $\pm$ 1.1 M$_{\odot}$ of $^{26}$Al and 1.7 $\pm$ 0.9 M$_{\odot}$ of $^{60}$Fe in the present interstellar medium. Predictions for the $^{60}$Fe mass distribution, total mass, and flux map are given, in particular a $^{60}$Fe / $^{26}$Al flux ratio of 0.16 $\pm$ 0.12. 26Al profile for a 25 Msun model 60Fe profile for a 25 Msun model 26Al & 60Fe profiles together Observations: The gamma-ray lines of 60Fe were measured by Smith (2004) using RHESSI and then by Wang et al (2007) using INTEGRAL. Both observations yield an $^{60}$Fe / $^{26}$Al flux ratio of 0.17 $\pm$ 0.05. Bouchet et al (2015) refine the INTEGRAL estimates to 0.14 $\pm$ 0.1. RHESSI 26Al measurement RHESSI 60Fe measurement Integral 60Fe measurement INTEGRAL 2015 map Integral Map Zoom Experiment: 60Fe decay scheme 60Fe lifetime measurement 26Al(n,α) measurement 26Al(n,p) measurement 60Fe(n,γ)61Fe cross section