Spatially resolved spectroscopy shows SDSS1335+0728 has a three-zone ionisation structure, optically thin dust, and sustained low-level nuclear activity for at least 1500 years, implying the Ansky event is a faint transient in an already accreting low-mass SMBH.
The Expulsion of Stellar Envelopes in Core-Collapse Supernovae
7 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
We examine the relation between presupernova stellar structure and the distribution of ejecta in core-collapse supernovae, assuming adiabatic, spherically symmetric flow. We develop a simple yet accurate formula for the blastwave shock velocity, and demonstrate that the entire final density distribution can be approximated with simple models for the final pressure distribution, along with the approximate shock-deposited entropy, in a way that matches the results of simulations. We find that the distribution of density in a star's ejecta depends on whether its outer envelope is radiative or convective, and if convective, on the composition structure of the star; simple approximate forms are presented for red and blue supergiant ejecta. Our models are most accurate for the high-velocity ejecta from the periphery of a star, where the shock dynamics are predictable. We present formulae for the final density distribution of this material, for both radiative and efficiently convective envelopes. These formulae limit to the well-known planar, self-similar solutions for mass shells approaching the stellar surface. But, the assumption of adiabatic flow fails at low optical depth, so this planar limit need not be attained. Formulae are given for the observable properties of the X-ray burst accompanying shock emergence, and their dependence on the parameters of the explosion. Motivated by the relativistic expansion recently inferred by Kulkarni et al. (1998) for the synchrotron shell around SN1998bw, we estimate the criterion for relativistic mass ejection and the rest mass of relativistic ejecta.
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Introduces a generalized fast framework for modeling interaction-powered transients with arbitrary CSM profiles and multi-wavelength outputs.
EP260321a/SN2026gzf is the first Type Ic-BL supernova with a likely X-ray shock breakout, and such bright breakouts may be rare.
SN 2019vxm is a luminous, long-lived Type IIn supernova showing early flash-ionization features, a power-law bolometric light curve, and mid-IR dust formation, with a progenitor mass-loss rate lower limit of at least 0.01 solar masses per year.
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.
Multi-shell modeling shows outward 56Ni mixing produces faster brighter rises and biases one-zone fits to lower ejecta mass and higher nickel fraction, while r-process signatures in collapsars depend on placement, distribution, and viewing angle rather than always showing NIR excess.
Analytical expressions for ALP-photon conversion in transient compact stars yield an updated bound g_aγ < 5×10^{-12} GeV^{-1} for m_a ≲ 10^{-9} eV from SN 1987A, plus sensitivity forecasts for future Galactic SN and NSM observations.
citing papers explorer
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Spatially resolved optical and mid-infrared spectroscopy of SDSS1335+0728: implications for the origin of the Ansky event
Spatially resolved spectroscopy shows SDSS1335+0728 has a three-zone ionisation structure, optically thin dust, and sustained low-level nuclear activity for at least 1500 years, implying the Ansky event is a faint transient in an already accreting low-mass SMBH.
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From mass-loss histories to lightcurves: a generalised framework for interaction-powered transients
Introduces a generalized fast framework for modeling interaction-powered transients with arbitrary CSM profiles and multi-wavelength outputs.
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A Multi-Wavelength View of the First Type Ic-BL Supernova with an Einstein Probe X-ray Shock Breakout
EP260321a/SN2026gzf is the first Type Ic-BL supernova with a likely X-ray shock breakout, and such bright breakouts may be rare.
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SN 2019vxm: A luminous and long-lived Type IIn supernova with early flash-ionisation features
SN 2019vxm is a luminous, long-lived Type IIn supernova showing early flash-ionization features, a power-law bolometric light curve, and mid-IR dust formation, with a progenitor mass-loss rate lower limit of at least 0.01 solar masses per year.
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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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Signatures of $^{56}$Ni Mixing and Neutron-rich Ejecta in Supernovae
Multi-shell modeling shows outward 56Ni mixing produces faster brighter rises and biases one-zone fits to lower ejecta mass and higher nickel fraction, while r-process signatures in collapsars depend on placement, distribution, and viewing angle rather than always showing NIR excess.
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Axion-photon conversion in transient compact stars: Systematics, constraints, and opportunities
Analytical expressions for ALP-photon conversion in transient compact stars yield an updated bound g_aγ < 5×10^{-12} GeV^{-1} for m_a ≲ 10^{-9} eV from SN 1987A, plus sensitivity forecasts for future Galactic SN and NSM observations.