Cococubed.com SN 1987A Light Curve
Home Astronomy research   Software Infrastructure:      MESA      FLASH-X      STARLIB      MESA-Web      starkiller-astro      My instruments   White dwarf pulsations:      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:      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 & Networks      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 Presentations Illustrations cococubed YouTube Bicycle adventures Public Outreach Education materials 2023 ASU Solar Systems Astronomy 2023 ASU Energy in Everyday Life AAS Journals AAS YouTube 2023 MESA VI 2023 MESA Marketplace 2023 MESA Classroom 2022 Earendel, A Highly Magnified Star 2022 White Dwarfs & 12C(α,γ)16O 2022 Black Hole Mass Spectrum 2022 MESA in Don't Look Up 2021 Bill Paxton, Tinsley Prize Contact: F.X.Timmes my one page vitae, full vitae, research statement, and teaching statement.	The light curve of SN 1987A revisited: constraining production masses of radioactive nuclides (2014) In this article, we revisit the evidence for the contribution of the long-lived radioactive nuclides $^{44}$Ti, $^{55}$Fe, $^{56}$Co, $^{57}$Co, and $^{60}$Co to the UVOIR light curve of SN 1987A. We show that the V-band luminosity constitutes a roughly constant fraction of the bolometric luminosity between 900 and 1900 days, and we obtain an approximate bolometric light curve out to 4334 days by scaling the late time V-band data by a constant factor where no bolometric light curve data is available. Considering the five most relevant decay chains starting at $^{44}$Ti, $^{55}$Co, $^{56}$Ni, $^{57}$Ni, and $^{60}$Co, we perform a least squares fit to the constructed composite bolometric light curve. For the nickel isotopes, we obtain best fit values of M($^{56}$Ni) = (7.1 $\pm$ 0.3) × 102 M⊙ and M($^{57}$Ni) = (4.1 $\pm$ 1.8) × 10-3 M⊙. Our best fit $^{44}$Ti mass is M($^{44}$Ti) = (0.55 $\pm$ 0.17) × 10-4 M⊙. which is in disagreement with the much higher (3.1 $\pm$ 0.8) × 10-4 M⊙ recently derived from INTEGRAL observations. The half-lives of $^{60}$Co and $^{55}$Fe are quite similar, which introduces a degeneracy for the fitting algorithm. As a result, we can only give upper limits on the relevant production masses of M($^{55}$Co) < 7.2 × 10-3 M⊙ and M($^{60}$Co) < 1.7 × 10-4 M⊙. Furthermore, we find that the leptonic channels in the decay of $^{57}$Co (internal conversion and Auger electrons) are a significant contribution and constitute up to 15.5% of the total luminosity. Consideration of the kinetic energy of these electrons is essential in lowering our best fit nickel isotope production ratio to [$^{57}$Ni / $^{56}$Ni] = 2.5$\pm$1.1 which is still somewhat high but in agreement with gamma-ray observations and model predictions. [57Ni / 56Ni] after freeze-out For canonically accepted values Including freeze-out corrections Importance of 57Co Best fit