Late-time data on SN 2017dio yield mass-loss rates of ~0.2 M_sun/yr peak and ~0.06 typical, with H-rich CSM from a companion and dust masses 0.001-0.02 M_sun, indicating sudden mass-loss increase.
Seeing the Collision of a Supernova with its Companion Star
3 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
The progenitors of Type Ia and some core collapse supernovae are thought to be stars in binary systems, but little observational evidence exists to confirm the hypothesis. We suggest that the collision of the supernova ejecta with its companion star should produce detectable emission in the hours and days following the explosion. The interaction occurs at distances ~10^11-10^13 cm and shocks the impacting supernova debris, dissipating kinetic energy and re-heating the gas. Initially, some radiation may escape promptly through the evacuated region of the shadowcone, producing a bright X-ray (0.1-2 keV) burst lasting minutes to hours with luminosity L ~ 10^44 ergs/s. Continuing radiative diffusion from deeper layers of shock heated ejecta produces a longer lasting optical/UV emission which exceeds the radioactively powered luminosity of the supernova for the first few days after the explosion. These signatures are prominent for viewing angles looking down upon the shocked region, or about 10% of the time. The properties of the emission provide a straightforward measure of the separation distance between the stars and hence (assuming Roche lobe overflow) the companion's radius. Current optical and UV data sets likely already constrain red giant companions. By systematically acquiring early time data for many supernovae, it should eventually be possible to empirically determine how the parameters of the progenitor system influence the outcome of the explosion.
years
2026 3verdicts
UNVERDICTED 3representative citing papers
GIGA-Lens 2.0 scales strong gravitational lens modeling across up to 128 GPU nodes and demonstrates it on 100 simulated systems plus one real DESI lens.
EP260321a is identified as the faintest shock breakout X-ray transient associated with broad-lined Ic supernova SN 2026gzf, interpreted as originating from a mildly relativistic weak outflow choked inside the progenitor star.
citing papers explorer
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Late-time evolution of the interacting stripped-envelope supernova 2017dio
Late-time data on SN 2017dio yield mass-loss rates of ~0.2 M_sun/yr peak and ~0.06 typical, with H-rich CSM from a companion and dust masses 0.001-0.02 M_sun, indicating sudden mass-loss increase.
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GIGA-Lens 2.0: Strong-Lens Modeling on Multiple GPU Nodes
GIGA-Lens 2.0 scales strong gravitational lens modeling across up to 128 GPU nodes and demonstrates it on 100 simulated systems plus one real DESI lens.
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EP260321a/SN 2026gzf: The Faintest Shock Breakout Associated with a Broad-Lined Supernova
EP260321a is identified as the faintest shock breakout X-ray transient associated with broad-lined Ic supernova SN 2026gzf, interpreted as originating from a mildly relativistic weak outflow choked inside the progenitor star.