Using 44Ti emission to differentiate between thermonuclear supernova progenitors

Daniel Kosakowski, Mark Ivan Ugalino, Robert Fisher, Or Graur, Alexey Bobrick, Hagai B. Perets

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Abstract

The radiosotope 44Ti is produced through α-rich freezeout and explosive helium burning in type Ia supernovae (SNe Ia). In this paper, we discuss how the detection of 44Ti, either through late-time light curves of SNe Ia, or directly via gamma rays, can uniquely constrain the origin of SNe Ia. In particular, building upon recent advances in the hydrodynamical simulation of helium-ignited double white dwarf binaries, we demonstrate that the detection of 44Ti in a nearby SN Ia or in a young galactic supernova remnant (SNR) can discriminate between the double-detonation and double-degenerate channels of sub-Chandrasekhar (sub-MCh) and near-Chandrasekhar (near-MCh) SNe Ia. In addition, we predict that the late-time light curves of calcium-rich transients are entirely dominated by 44Ti.
Original languageEnglish
Pages (from-to)L74-L78
Number of pages5
JournalMonthly Notices of the Royal Astronomical Society
Volume519
Issue number1
Early online date28 Nov 2022
DOIs
Publication statusPublished - 1 Feb 2023

Keywords

  • astro-ph.HE
  • astro-ph.SR
  • nuclear reactions
  • nucleosynthesis
  • abundances
  • white dwarfs
  • transients: supernovae

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