Cococubed.com MeV Gamma-Rays From Supernovae
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 & 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 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.	Gamma-Ray Line Signals from Supernovae within 100 Mpc (1997) The average number of supernovae per year detectable by $\gamma$-rays emitted during the decay of $^{56}$Ni to $^{56}$Fe is estimated in this article for galaxies within 100 Mpc as a function of limiting sensitivity using standard supernova yields and the Sternberg and Asiago supernova catalogs. An instrument having a broad line (5000 km s$^{-1}$) sensitivity of $2 \times 10^{-6}$ $\gamma$ s$^{-1}$ cm$^{-2}$ should detect a minimum of \hbox{1.0 $\pm$ 0.5} Type Ia supernova per year, and observe all Type Ia events from the Virgo, Fornax, and possibly the Hydra galaxy clusters. Roughly 10-30% of all Type Ia supernova within 100 Mpc are detectable at this flux sensitivity. Instruments having broad line flux sensitivities larger than $1.5 \times 10^{-5}$ $\gamma$ s$^{-1}$ cm$^{-2}$ will probably only detect rare Type Ia supernovae within 10 Mpc, such as SN 1972E or SN 1991T. Flux sensitivities of $\simeq 2 \times 10^{-6}$ $\gamma$ s$^{-1}$ cm$^{-2}$ to intermediate width $\gamma$-ray lines should enable the detection of a minimum of 0.2 $\pm$ 0.2 Type Ib/c supernova per year, and easily allow events similar to SN 1983N and SN 1985F to be seen. Instruments of the near future will not detect the narrow line $\gamma$-rays from any Type II supernovae that originate beyond the Local Group of galaxies. These number and rate estimates provide guidelines for the design of future $\gamma$-ray missions. Supernova Type Ia Type 1a SN per year How far away are they? Expected fluxes Type Ia detection rates Supernova Type Ib/c Type 1b/c SN per year How far away are they? Expected fluxes Type Ib/c detection rates Supernova Type II Type II SN per year How far away are they? Expected fluxes Type II detection rates