A new gravitational wave event reveals a binary black hole merger with total mass 190-265 solar masses, indicating black holes can form via gravitational-wave driven mergers beyond standard stellar channels.
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E., Heger A., Weaver T
34 Pith papers cite this work. Polarity classification is still indexing.
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JWST spectra of SN 2024abup show CO, C, O, and Mg features plus possible dust emission, with no clear r-process signatures identified via SUMO modeling.
Binary interactions and cluster dynamics boost PISN rates by up to 3x versus single stars, enabling constraints on stellar-wind mass loss and galaxy metallicity distributions.
MOFAT applied to SN2024ggi shows CO triggering inner SiO formation with a receding edge, order-of-magnitude mass drop, clumping signatures, and no dust formation.
Super-Kamiokande's SNWATCH system now delivers supernova direction alerts in about 90 seconds via a new fast HEALPix fitter and an upgraded maximum-likelihood fitter that incorporates gadolinium data.
SN 2020bij and four other Type IIP SNe with slow-rising light curves and high velocities are modeled with weak to no CSM interaction, suggesting a new subclass linked to confined CSM.
JWST spectra of SN 2022acko reveal CO masses of 1.55e-4 and 2.47e-4 solar masses, IME velocities ~300 km/s vs ~100 km/s for H/He/IGEs suggesting bipolar outflow, and substantially less molecule formation than higher-mass Type II SNe.
Presents a grid of 113 fast-rotating, chemically-homogeneous massive star models at Z=0.001 reaching core collapse with high angular momentum for use as supernova and GRB progenitors.
Physics-based annual TSI reconstruction over three millennia yields a maximum difference of 1.04 W/m² in 50-year running means.
Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.
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.
Efficient mass transfer in binaries naturally limits the mass of the first-born black hole and produces a sharp drop above 45 solar masses that mimics the pair-instability gap.
Quasinormal modes for three spin fields on Einstein-Skyrme AdS black holes exhibit a mild overtone anomaly and confirm strong cosmic censorship with Christodoulou parameter β much smaller than 1/2.
The upper edge of the PISN black hole mass gap shifts by up to 30 solar masses due to nuclear reaction rate uncertainties, primarily the 12C(α,γ)16O rate, while remaining robust to resolution variations unlike the lower edge.
A 1D accretion model shows MAD formation for Pm ≳ 1, outer-disk IR emission missed by one-zone approximations, and Pm-dependent X-ray mechanisms that affect IBH detectability in dense clouds.
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.
Semi-analytical models show AGN disks produce repeated BBH mergers with a high-mass tail beyond the pair-instability gap, more efficiently at low viscosity, with spin and mass-ratio signatures that can match events like GW190521.
New 59Fe beta-decay rates in non-rotating MESA models suppress 60Fe yields by 0.28 dex, yielding a Salpeter-IMF-integrated 60Fe/26Al flux ratio of 0.18 that matches the observed 0.184 ± 0.042.
SN 2020aze displays early He II emission from ejecta-CSM interaction, a steep V-band decline, and semi-analytical modeling yields a ~14 solar-mass red supergiant progenitor with ~12 solar-mass ejecta and 1.5e51 erg explosion energy.
Stellar evolution and atmosphere models predict black hole progenitors are predominantly hot and blue with a direct-collapse rate of ~0.4 per century in a 1 Msun/yr star-forming galaxy.
Core-collapse supernova models including C-O shell mergers best match observed elemental ratios in Cas A, indicating mergers occur and contribute up to 20-30% of 44Ti outside the reverse shock.
New CCSN yield tables at varying metallicities are inserted into galactic chemical evolution models and tuned to reproduce the Si-group and Fe-group abundances measured by Hitomi in the Perseus Cluster.
SLSN 2021bnw is best fit by a core-collapse explosion of a star with initial mass at least 61 solar masses, ejecta of 15-22.5 solar masses containing 1.7 solar masses of nickel-56 and 4 foe energy colliding with 7 solar masses of circumstellar matter.
citing papers explorer
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JWST observations of SN 2024abup: First Detection of CO in a broad-lined Type Ic Supernova and Constraints on r-process Nucleosynthesis
JWST spectra of SN 2024abup show CO, C, O, and Mg features plus possible dust emission, with no clear r-process signatures identified via SUMO modeling.
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The impact of stellar binaries and star cluster dynamics on pair-instability supernovae
Binary interactions and cluster dynamics boost PISN rates by up to 3x versus single stars, enabling constraints on stellar-wind mass loss and galaxy metallicity distributions.
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Probing the 3D Structures of Supernovae through IR Signatures of CO and SiO
MOFAT applied to SN2024ggi shows CO triggering inner SiO formation with a receding edge, order-of-magnitude mass drop, clumping signatures, and no dust formation.
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SN 2020bij and a Possible Slow-Rise High-Velocity Subclass of Type IIP Supernovae
SN 2020bij and four other Type IIP SNe with slow-rising light curves and high velocities are modeled with weak to no CSM interaction, suggesting a new subclass linked to confined CSM.
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JWST Medium-Resolution Infrared Spectroscopy of SN 2022acko: Tracing Molecule Formation in the Nebular Phase
JWST spectra of SN 2022acko reveal CO masses of 1.55e-4 and 2.47e-4 solar masses, IME velocities ~300 km/s vs ~100 km/s for H/He/IGEs suggesting bipolar outflow, and substantially less molecule formation than higher-mass Type II SNe.
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A grid of fast-rotating, chemically-homogeneous, supernova and/or long-GRB progenitors
Presents a grid of 113 fast-rotating, chemically-homogeneous massive star models at Z=0.001 reaching core collapse with high angular momentum for use as supernova and GRB progenitors.
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Reconstruction of annual solar irradiance over the last three millennia
Physics-based annual TSI reconstruction over three millennia yields a maximum difference of 1.04 W/m² in 50-year running means.
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Massquerade: Impacts of Mass Ratio Reversals on Binary Black Hole Merger Rates and Mass Distributions
Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.
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Binary Evolution Can Mimic the Pair-Instability Mass Gap in Black Hole Mergers
Efficient mass transfer in binaries naturally limits the mass of the first-born black hole and produces a sharp drop above 45 solar masses that mimics the pair-instability gap.
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The location of the upper edge of the pair-instability supernovae black hole mass gap
The upper edge of the PISN black hole mass gap shifts by up to 30 solar masses due to nuclear reaction rate uncertainties, primarily the 12C(α,γ)16O rate, while remaining robust to resolution variations unlike the lower edge.
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Multi-wavelength Emission Modeling from Accretion Flows around Isolated Black Holes Including Magnetic Flux Transport
A 1D accretion model shows MAD formation for Pm ≳ 1, outer-disk IR emission missed by one-zone approximations, and Pm-dependent X-ray mechanisms that affect IBH detectability in dense clouds.
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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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AGN-driven BBH mergers: Black hole populations and hierarchical growth across the AGN parameter space
Semi-analytical models show AGN disks produce repeated BBH mergers with a high-mass tail beyond the pair-instability gap, more efficiently at low viscosity, with spin and mass-ratio signatures that can match events like GW190521.
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Early interaction signatures and an extended plateau phase in Type II SN 2020aze
SN 2020aze displays early He II emission from ejecta-CSM interaction, a steep V-band decline, and semi-analytical modeling yields a ~14 solar-mass red supergiant progenitor with ~12 solar-mass ejecta and 1.5e51 erg explosion energy.
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Hot blue progenitors of stellar-mass black holes
Stellar evolution and atmosphere models predict black hole progenitors are predominantly hot and blue with a direct-collapse rate of ~0.4 per century in a 1 Msun/yr star-forming galaxy.
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Production of heavy $\alpha$-elements and $^{44}$Ti in Cas A: comparison to abundances from 1D core-collapse supernova models and evidence for Carbon-Oxygen shell mergers
Core-collapse supernova models including C-O shell mergers best match observed elemental ratios in Cas A, indicating mergers occur and contribute up to 20-30% of 44Ti outside the reverse shock.
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Revisiting the Perseus Cluster II: Metallicity-Dependence of Massive Stars and Chemical Enrichment History
New CCSN yield tables at varying metallicities are inserted into galactic chemical evolution models and tuned to reproduce the Si-group and Fe-group abundances measured by Hitomi in the Perseus Cluster.
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Helium superluminous SN 2021bnw : an explosion of a massive star with a pre-outburst
SLSN 2021bnw is best fit by a core-collapse explosion of a star with initial mass at least 61 solar masses, ejecta of 15-22.5 solar masses containing 1.7 solar masses of nickel-56 and 4 foe energy colliding with 7 solar masses of circumstellar matter.
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The impact of asymmetric neutrino emissions on nucleosynthesis in core-collapse supernovae
Asymmetric neutrino emissions produce proton-rich ejecta in one hemisphere and neutron-rich ejecta in the other, with asymmetries of 30% or more overproducing elements heavier than zinc relative to solar abundances.
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SN 2023rve: A Type II Supernova with No Nebular Oxygen
SN 2023rve exhibits absent [O I] nebular lines with inferred 14-18 solar mass progenitor, 0.27e51 erg explosion energy, and 0.0064 solar mass nickel, possibly indicating partial fallback.
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The Eye of Sauron in SN 2025ngs: a Short-plateau Cousin of SN 1998S with Evidence for a Ring-like Circumstellar Medium
SN 2025ngs is a short-plateau supernova resembling SN 1998S but fainter, with spectral evidence for interaction with a proximate ring-like circumstellar medium around a supergiant progenitor.
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Revisiting the Rhoades-Ruffini bound
Relaxing the onset assumption for stiff high-density matter raises the theoretical maximum neutron star mass to 4 solar masses or higher.
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The impact of new ($\alpha$, n) reaction rates on the weak s-process in metal-poor massive stars
New 17O+α and 22Ne+α rates increase weak s-process yields by tens of times in Z=10^{-3} stars of 15-30 solar masses.
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Chemical abundances in the metal-intermediate GC NGC 6723
New abundance measurements for NGC 6723 align its chemical patterns with other metal-intermediate globular clusters rather than indicating a transition to metal-rich properties.
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Supernovae with the Square Kilometre Array
This review chapter updates prior work to outline the SKA's expected role in turning radio observations of supernovae into population statistics through wide-field surveys and targeted follow-up.
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Can current models predict the local black hole merger rate?
Theoretical predictions for local BBH merger rates exceed observations by a factor >10 under conservative SFRD and metallicity assumptions, indicating need for revisions in stellar evolution.