Using 44Ti emission to differentiate between thermonuclear supernova progenitors

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

doi:10.1093/mnrasl/slac152

Using ⁴⁴Ti emission to differentiate between thermonuclear supernova progenitors

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

Institute of Cosmology & Gravitation

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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-M_Ch) and near-Chandrasekhar (near-M_Ch) SNe Ia. In addition, we predict that the late-time light curves of calcium-rich transients are entirely dominated by ⁴⁴Ti.

Original language	English
Pages (from-to)	L74-L78
Number of pages	5
Journal	Monthly Notices of the Royal Astronomical Society
Volume	519
Issue number	1
Early online date	28 Nov 2022
DOIs	https://doi.org/10.1093/mnrasl/slac152
Publication status	Published - 1 Feb 2023

Keywords

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

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10.1093/mnrasl/slac152

Using 44Ti emission PDF
This article has been accepted for publication in MNRAS ©: 2022 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
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Cite this

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title = "Using 44Ti emission to differentiate between thermonuclear supernova progenitors",

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. ",

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AU - Kosakowski, Daniel

AU - Ugalino, Mark Ivan

AU - Fisher, Robert

AU - Graur, Or

AU - Bobrick, Alexey

AU - Perets, Hagai B.

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KW - astro-ph.SR

KW - nuclear reactions

KW - nucleosynthesis

KW - abundances

KW - white dwarfs

KW - transients: supernovae

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