Simulations predict time-dependent gamma-ray lines from r-process and iron-peak decays in accretion-induced white dwarf collapse, detectable to ~10 Mpc and absent in neutron star mergers.
Collapse of Magnetized White Dwarfs as site of Heavy Element Formation and Kilonova Signal
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abstract
We present the first end-to-end calculation connecting the accretion-induced collapse (AIC) of a magnetized, rapidly rotating white dwarf to observable kilonova signatures, combining 2D general-relativistic neutrino-magnetohydrodynamic simulations, followed by radiation hydrodynamics with in-situ nuclear network and 2D Monte Carlo radiative transfer with spatially resolved heating rates. Unlike all previous unmagnetized AIC models - which predicted proton-rich, $^{56}$Ni-dominated ejecta - strong magnetic fields eject ${\sim 0.2 M_\odot}$ of neutron-rich material $(\langle Y_e \rangle \sim 0.24)$ on dynamical timescales, before neutrino irradiation can raise the electron fraction, enabling strong $r$-process nucleosynthesis up to and beyond the third peak. The resulting kilonova is lanthanide-rich $(X_{\rm lan} \approx 8\%)$ and dominated by near-infrared emission. We compute synthetic light curves in the LSST and JWST bands and find striking agreement, without parameter tuning, between the observations of AT 2023vfi/GRB 230307A and our broadband light curves for polar viewing angles. These results establish magnetized AIC as a viable channel for heavy $r$-process element production and a compelling progenitor candidate for long-duration gamma-ray bursts with kilonova signatures.
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UNVERDICTED 5representative citing papers
Dust from refractory r-process elements forms efficiently in kilonova ejecta and explains the observed late-time infrared spectra.
Binary neutron star mergers with evolving merger rates or yields are strongly preferred over constant scenarios to explain Milky Way r-process enrichment, with Bayes factors exceeding 10^20, yet remain in tension with short gamma-ray burst observations.
Relativistic outflows in accretion-induced collapse of white dwarfs are modeled as sources of UHECRs, contributing a few 10^43-10^45 erg Mpc^{-3} yr^{-1} assuming iron-like nuclei and sufficient event rates.
Magnetorotational r-process best explains lighter elements and CEJSN explains the third peak based on scatter and iron correlations in early metal-poor stars.
citing papers explorer
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Gamma-ray Signatures of r-Process Radioactivity from the Collapse of Magnetized White Dwarfs
Simulations predict time-dependent gamma-ray lines from r-process and iron-peak decays in accretion-induced white dwarf collapse, detectable to ~10 Mpc and absent in neutron star mergers.
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Heavy element dust explains the late-time spectra of kilonovae
Dust from refractory r-process elements forms efficiently in kilonova ejecta and explains the observed late-time infrared spectra.
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Binary Neutron Star Merger Evolution and r-Process Enrichment in the Milky Way Disk
Binary neutron star mergers with evolving merger rates or yields are strongly preferred over constant scenarios to explain Milky Way r-process enrichment, with Bayes factors exceeding 10^20, yet remain in tension with short gamma-ray burst observations.
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Ultra high-energy cosmic rays from relativistic outflows in accretion induced collapse of white dwarfs
Relativistic outflows in accretion-induced collapse of white dwarfs are modeled as sources of UHECRs, contributing a few 10^43-10^45 erg Mpc^{-3} yr^{-1} assuming iron-like nuclei and sufficient event rates.
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The early r-process nucleosynthesis scenarios
Magnetorotational r-process best explains lighter elements and CEJSN explains the third peak based on scatter and iron correlations in early metal-poor stars.