Collapse of Magnetized White Dwarfs as site of Heavy Element Formation and Kilonova Signal

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ID: 313626
2026
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Abstract
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, 56Ni-dominated ejecta—strong magnetic fields eject ≈ 0.2 M⊙ of neutron-rich material (〈Ye〉 ~ 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 (Xlan ≈ 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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Authors Tetyana Pitik, David Radice, Daniel Kasen, Fabio Magistrelli, Patrick Chi-Kit Cheong, Sebastiano Bernuzzi
Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag899
URL
https://doi.org/10.1093/mnras/stag899
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