Quantitative Bayesian inference using a deep-learning emulator detects 0.018-0.020 M_sun of helium in the Type Ic supernova 2014L.
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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.
3D hydro simulations demonstrate that donor central concentration (ρ_c/ρ_bar) controls inspiral morphology and mass-ejection history in common-envelope events for luminous red novae.
Severe gas expulsion and expansion in a primordial star cluster, combined with a top-heavy IMF, can reproduce the high velocity dispersion and broad stream of C-19 without dark matter subhalos.
Type Ib supernovae are systematically bluer than Type Ic supernovae in optical colors, likely due to helium-rich versus helium-poor progenitors.
Simulations find nested bow shocks around an engulfed neutron star enhance drag force 10-100 times over Bondi-Hoyle-Lyttleton and allow force reversal based on envelope conditions.
Radio and X-ray data on four old Type IIn supernovae show mass-loss rates 1-2 orders of magnitude below optical estimates, indicating rapidly evolving progenitor winds over the final centuries before explosion.
Models BBH spin-orbit alignment as random walk on sphere, deriving exact distribution after n encounters and showing alignment survives several strong encounters before isotropy.
Disrupted dense star clusters release ~300,000 white dwarf, 150,000 black hole, and 1,000 neutron star binaries into the Milky Way, but Gaia DR3/DR4 detect only a handful of white dwarf systems with none for the others.
New spectral models of solar-metallicity stellar populations using POSYDON show binary-stripped stars dominating ionizing radiation after about 16 Myr.
A parametrized analytical model for BBH mass ratios from the stable mass transfer channel is derived and applied to the 10 solar-mass peak in GWTC-4, favoring little mass-ratio reversal.
Physics-based annual TSI reconstruction over three millennia yields a maximum difference of 1.04 W/m² in 50-year running means.
Blue-asymmetric spectral lines appear in 50-60% of dense cores within massive dark clumps, showing that gravitational collapse operates at core scales from prestellar stages onward and supports hierarchical star formation.
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.
Radial velocity data reveal a 310-day orbital period in NaSt1 with opposing phases in two groups of emission lines, supporting its nature as a post-mass-transfer massive binary system.
Dynamical dissolution of soft primordial binaries fully explains observed main-sequence binary fractions in globular clusters under solar-neighborhood initial conditions.
A new main-sequence evolution framework implemented in COMPAS yields more massive helium cores, more compact stripped-star radii, and systematically higher black-hole masses than standard prescriptions.
New MESA stellar tracks with varied winds and convective mixing produce a primary black hole mass function with twin peaks near 8 and 13 solar masses in most variations, the higher peak dominated by mass-ratio-reversal systems, with rates varying by a factor of six.
Stable mass transfer produces two distinct peaks in merging binary black hole primary mass and mass ratio distributions via mass ratio reversal under conservative mass transfer.
Multi-wavelength observations of SN 2019vxm trace three phases of shock interaction in a Type IIn supernova, estimating CSM mass of 3-8 solar masses and ejecta mass of ~3.88 solar masses with late-time dust signatures.
Spectropolarimetry of SN 2026gzf indicates mostly spherical ejecta with axisymmetric Ca distribution viewed at ~40° from symmetry axis.
1D models show convective boundary mixing dominates the asteroseismic imprint of accretion in massive stars, robust to semiconvection changes but drastically altered without it, with thermal relaxation as key.
Failed common envelope mergers yield 6-14 solar mass stripped stars consistent with long-lived core He-burning objects that appear single or in wide binaries from hierarchical triples.
Observational analysis of EMP stars including a new r-process enhanced star G256353 whose heavy-element pattern matches scaled solar and neutron-star-merger predictions, supporting r-process universality.
citing papers explorer
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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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Hydrodynamic Response of Mildly Evolved Common Envelope Donors in Luminous Red Novae
3D hydro simulations demonstrate that donor central concentration (ρ_c/ρ_bar) controls inspiral morphology and mass-ejection history in common-envelope events for luminous red novae.
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The formation of the C-19 progenitor: a primordial cluster heated by gas expulsion
Severe gas expulsion and expansion in a primordial star cluster, combined with a top-heavy IMF, can reproduce the high velocity dispersion and broad stream of C-19 without dark matter subhalos.
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Type Ib Supernovae are bluer than Type Ic Supernovae
Type Ib supernovae are systematically bluer than Type Ic supernovae in optical colors, likely due to helium-rich versus helium-poor progenitors.
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Numerical Studies of Accretion Flows onto a Neutron Star Engulfed in a Massive Star
Simulations find nested bow shocks around an engulfed neutron star enhance drag force 10-100 times over Bondi-Hoyle-Lyttleton and allow force reversal based on envelope conditions.
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Fading Echoes of Interaction: Probing Centuries of Preexplosion Mass-Loss in Four Type IIn Supernovae
Radio and X-ray data on four old Type IIn supernovae show mass-loss rates 1-2 orders of magnitude below optical estimates, indicating rapidly evolving progenitor winds over the final centuries before explosion.
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Getting Tilted: Random Walk of Binary Black Hole Spin-Orbit Alignment in Dense Star Clusters
Models BBH spin-orbit alignment as random walk on sphere, deriving exact distribution after n encounters and showing alignment survives several strong encounters before isotropy.
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The Contribution of Disrupted Dense Star Clusters to Gaia's Compact Object Binaries
Disrupted dense star clusters release ~300,000 white dwarf, 150,000 black hole, and 1,000 neutron star binaries into the Milky Way, but Gaia DR3/DR4 detect only a handful of white dwarf systems with none for the others.
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Stellar Population Spectra Incorporating Detailed Binary Evolution using POSYDON
New spectral models of solar-metallicity stellar populations using POSYDON show binary-stripped stars dominating ionizing radiation after about 16 Myr.
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A Strongly Parametrized Mass Ratio Model for the Stable Mass Transfer Channel: a Case Study of the $10 \, \rm{M}_{\odot}$ Peak
A parametrized analytical model for BBH mass ratios from the stable mass transfer channel is derived and applied to the 10 solar-mass peak in GWTC-4, favoring little mass-ratio reversal.
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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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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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Evolution of Massive Main-sequence Stars in Rapid Population Synthesis. I. Framework and Implementation
A new main-sequence evolution framework implemented in COMPAS yields more massive helium cores, more compact stripped-star radii, and systematically higher black-hole masses than standard prescriptions.
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A Stellar Role Reversal: Multiple Features in the Mass and Mass Ratio Distributions of Merging Binary Black Holes from Stable Mass Transfer
Stable mass transfer produces two distinct peaks in merging binary black hole primary mass and mass ratio distributions via mass ratio reversal under conservative mass transfer.
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Two years of shock interaction tracing three phases of evolution: the explosion of a Type IIn supernova, SN 2019vxm
Multi-wavelength observations of SN 2019vxm trace three phases of shock interaction in a Type IIn supernova, estimating CSM mass of 3-8 solar masses and ejecta mass of ~3.88 solar masses with late-time dust signatures.
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Pinning Down the Geometry of the Type Ic Broad-Line Supernova 2026gzf
Spectropolarimetry of SN 2026gzf indicates mostly spherical ejecta with axisymmetric Ca distribution viewed at ~40° from symmetry axis.
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The effect of near-core mixing on rejuvenation and the asteroseismic properties of massive accretors
1D models show convective boundary mixing dominates the asteroseismic imprint of accretion in massive stars, robust to semiconvection changes but drastically altered without it, with thermal relaxation as key.
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Mergers via failed common envelope as a route towards intermediate-mass stripped stars
Failed common envelope mergers yield 6-14 solar mass stripped stars consistent with long-lived core He-burning objects that appear single or in wide binaries from hierarchical triples.
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The \emph{R}-process Alliance: A Bright, Strongly \emph{R}-process-enhanced Extremely Metal-poor Star Observed with GHOST
Observational analysis of EMP stars including a new r-process enhanced star G256353 whose heavy-element pattern matches scaled solar and neutron-star-merger predictions, supporting r-process universality.
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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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Adiabatic Mass Loss In Binary Stars. VI. Massive Helium Binary Stars
Adiabatic mass-loss models for massive helium stars give critical mass ratios 0.7-3.0 on the main sequence and 1.5-27 on the Hertzsprung gap, lowered by winds and adjusted by isotropic re-emission.
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Formation and disruption of wide binaries in star clusters revealed by N-body simulations
N-body simulations show wide binaries disrupt rapidly in the first 10 Myr due to high-density encounters, with semi-analytical models matching the evolution and identifying young low-density clusters as optimal detection sites.
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Radiatively Cooled Binary Mass Transfer: Flow Structure, Luminosities, and L2 Outflows Across Mass Transfer Rates
Simulations across mass transfer rates from 10^-5 to 10^-1 solar masses per year find that radiatively cooled binaries develop equatorially concentrated L2 outflows and increasing cooling luminosity at high rates.
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Red vs. Blue: How metallicity shapes black hole dynamics and mergers in dense star clusters
High-metallicity star cluster simulations produce black hole mergers with masses and ratios consistent with recent LVK detections, unlike low-metallicity models.
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Comparative Study of Two Luminous Red Novae I. Progenitor Modeling and Dust Formation
Binary evolution modeling constrains donor masses of 14-23 solar masses for two luminous red novae and shows dust masses are 1-5 orders of magnitude below total ejected envelope masses.
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Exploring biases in derived stellar parameters and the ionizing photon production efficiency
Different SED fitting techniques and data types produce stellar parameters and xi_ion values differing by up to 1.1 dex even for a homogeneous sample of z=3 EoR-analog galaxies, with apparent redshift evolution of xi_ion appearing only under consistent methodology.
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Long-term optical and near-infrared photometric evolution of SN 2019vxm, an interacting Type IIn supernova
Long-term multi-band photometry of SN 2019vxm shows initial thick CSM interaction, photosphere decoupling at 80-100 days, long-lasting dust emission, and a possible outer CSM rebrightening, implying a massive progenitor with extreme pre-explosion mass loss.
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Contribution of interstellar objects to local dark matter density
Interstellar objects may contribute enough baryonic mass to reduce the local dark matter halo density to 0.24 GeV/cm³.
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Star cluster formation from turbulent clumps. V. Stellar clustering around massive stars
N-body simulations show massive stars in TCCA clusters rapidly acquire triple or higher multiples and local density enhancements via dynamics, with multiplicity trends and shallower N_* profiles than competitive accretion models, matching AFGL 5180 better.
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A Path to Constraints on Common Envelope Ejection in Massive Binaries: Full Evolutionary Reconstruction of Three Black Hole X-ray Binaries
Reconstruction of GRO J1655-40, SAX J1819.3-2525 and 4U 1543-47 requires CE efficiencies α_0.5U ≳6.7, α_U ≳4.2, α_H ≳1.7 with no solutions below unity, implying need for additional energy or formalism changes plus natal kicks ≳50 km/s for 4U 1543-47.