Late-time IR spectroscopy of SN 2024ggi shows varied line morphologies implying chemical inhomogeneity and aspherical ionization, with modeling favoring 12-15 solar mass progenitors but only high-mass energetic 3D simulations matching the observed Ni mixing extent.
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XSNAP provides a unified pipeline for X-ray supernova analysis and derives a progenitor mass-loss rate of (6.2±0.2)×10^{-5} solar masses per year for SN 2024ggi assuming a 20 km/s wind.
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Mapping 3-D Explosive Nucleosynthesis with Type II Supernova Infrared Emission Lines
Late-time IR spectroscopy of SN 2024ggi shows varied line morphologies implying chemical inhomogeneity and aspherical ionization, with modeling favoring 12-15 solar mass progenitors but only high-mass energetic 3D simulations matching the observed Ni mixing extent.
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XSNAP: An X-ray Supernova Analysis Pipeline with Application to the Type II Supernova 2024ggi
XSNAP provides a unified pipeline for X-ray supernova analysis and derives a progenitor mass-loss rate of (6.2±0.2)×10^{-5} solar masses per year for SN 2024ggi assuming a 20 km/s wind.