Synthetic observables from tECSN models show slower early red-color decline due to higher Ti/Cr and a late-time 12.8 μm Ne II line that strengthens over time, unlike comparable CO deflagration models.
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23 Pith papers cite this work, alongside 1,066 external citations. Polarity classification is still indexing.
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Bayesian framework with active-learning surrogate for MESA models constrains ages and α_MLT from 38 main-sequence DEBs, recovering some α_MLT values below the solar calibration.
Self-consistent spherical accretion simulations show cooling-enhanced growth of PBHs with radiative efficiency ~10^{-2} in the bremsstrahlung regime, yielding a critical seed mass of ~10^{-16} M_sun to consume a solar-mass star in a Hubble time.
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.
Simulations show magnetar giant flares produce nuclei near r-process peaks whose decays create bright MeV gamma-ray lines from 88Kr and 92Sr with fluxes above 10^-8 erg cm^-2 s^-1.
Population synthesis from binary evolution models predicts periodic neutron star-companion interactions in more than half of surviving hydrogen-poor core-collapse supernovae, with periods peaking at 20-50 days and lasting 0.5-10 years.
3D simulations find that the convective Urca process reduces mixing efficiency near the convective boundary in a simmering white dwarf but does not restrict the overall size of the convection zone, with the A=23 pair having the largest effect.
Multi-D progenitor perturbations leave shock revival and explosion energetics essentially unchanged in 2D CHIMERA runs; any effects sit below the level of numerical stochasticity.
3D simulations show the convective Urca process substantially reduces the convection zone size in a simmering white dwarf, though convection extends past the Urca shell.
Long-term 3D CCSN simulations of a low-mass iron-core progenitor show NS wind and multi-isotope decay heating create large plumes, asymmetric breakout, reverse-shock fragmentation, and ECSN-like yields unlike Cas A.
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.
MESA simulations show that winds from Type I X-ray bursts igniting at column depths ≥5×10^8 g cm^{-2} eject ash enriched in intermediate-mass to iron-peak elements, with composition depending on ignition depth, accretion mix, and convective treatment.
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.
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.
The paper develops a search algorithm to find observable MeV gamma-ray peaks from r-process isotope decays in mergers and shows Rh-106 can distinguish main versus weak r-process while Tl-208 remains robust across model variations.
Free neutrons survive r-process freeze-out in fast ejecta of neutron star mergers and their beta-decay heating produces a visible early kilonova precursor for mass fractions above ~0.05.
The first NIR high-resolution spectroscopy of solar analog HD115617 shows a 250 K temperature discrepancy with optical data but confirms solar composition, main-sequence status, and no chemical signature of planetary formation.
Stellar models show that the 12C(alpha,gamma)16O rate uncertainty moves the black hole mass gap, constraining its S300 to 137.6-263.4 keV barn when matched to the observed gap from gravitational waves.
Rotation produces only modest changes to blue loop luminosity and extent in MESA Cepheid models and cannot fix the mass discrepancy without substantial main-sequence overshooting.
Type Ib supernovae are systematically bluer at optical peak than Type Ic supernovae, suggesting their progenitors contain more helium.
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.
MESA grids show global magnetic sensitivity in red giants depends on mass and metallicity and can be recovered to 10% uncertainty with accurate spectroscopic metallicity.
Binary evolution simulations identify short (20-500 days) and long (2000-4000 days) orbital period ranges where massive star-black hole systems retain enough angular momentum for GRB jet production with negligible mass loss.
citing papers explorer
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Observational signatures of thermonuclear electron-capture supernovae -- Ne II line strengthening and color evolution as traces of the explosion mechanism
Synthetic observables from tECSN models show slower early red-color decline due to higher Ti/Cr and a late-time 12.8 μm Ne II line that strengthens over time, unlike comparable CO deflagration models.
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Precision constraints on stellar physics from main sequence detached eclipsing binaries
Bayesian framework with active-learning surrogate for MESA models constrains ages and α_MLT from 38 main-sequence DEBs, recovering some α_MLT values below the solar calibration.
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Accretion of Primordial Black Holes in Stellar Interiors
Self-consistent spherical accretion simulations show cooling-enhanced growth of PBHs with radiative efficiency ~10^{-2} in the bremsstrahlung regime, yielding a critical seed mass of ~10^{-16} M_sun to consume a solar-mass star in a Hubble time.
-
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.
-
MeV Gamma-Ray Lines from Radioactive Nuclei in Magnetar Giant Flares
Simulations show magnetar giant flares produce nuclei near r-process peaks whose decays create bright MeV gamma-ray lines from 88Kr and 92Sr with fluxes above 10^-8 erg cm^-2 s^-1.
-
Neutron star-companion interaction in core collapse supernovae. Population synthesis based on detailed binary evolution models
Population synthesis from binary evolution models predicts periodic neutron star-companion interactions in more than half of surviving hydrogen-poor core-collapse supernovae, with periods peaking at 20-50 days and lasting 0.5-10 years.
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Simulating the Convective Urca Process with Multiple Urca Pairs in a Simmering White Dwarf
3D simulations find that the convective Urca process reduces mixing efficiency near the convective boundary in a simmering white dwarf but does not restrict the overall size of the convection zone, with the A=23 pair having the largest effect.
-
Impacts of Multidimensional Progenitor Perturbations on Core-Collapse Supernova Explosions
Multi-D progenitor perturbations leave shock revival and explosion energetics essentially unchanged in 2D CHIMERA runs; any effects sit below the level of numerical stochasticity.
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On the Importance of the Convective Urca Process in 3D Simulations of a Simmering White Dwarf
3D simulations show the convective Urca process substantially reduces the convection zone size in a simmering white dwarf, though convection extends past the Urca shell.
-
Simulation to a Newborn Supernova Remnant from a Low-mass Iron Core Star
Long-term 3D CCSN simulations of a low-mass iron-core progenitor show NS wind and multi-isotope decay heating create large plumes, asymmetric breakout, reverse-shock fragmentation, and ECSN-like yields unlike Cas A.
-
Twin Peaks: Resolving Features in the Binary Black Hole Mass Function with COSMIC-METISSE
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.
-
Composition of Radiation-Driven Winds from Type I X-ray Bursts
MESA simulations show that winds from Type I X-ray bursts igniting at column depths ≥5×10^8 g cm^{-2} eject ash enriched in intermediate-mass to iron-peak elements, with composition depending on ignition depth, accretion mix, and convective treatment.
-
The Impact of the New $^{59}$Fe Decay Rates on $^{60}$Fe and $^{26}$Al Nucleosynthesis in Massive Stars
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.
-
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.
-
Identifying observable MeV lines from the decays of weak and main $r$-process isotopes in mergers
The paper develops a search algorithm to find observable MeV gamma-ray peaks from r-process isotope decays in mergers and shows Rh-106 can distinguish main versus weak r-process while Tl-208 remains robust across model variations.
-
Nucleosynthesis in the fast ejecta of a neutron star merger
Free neutrons survive r-process freeze-out in fast ejecta of neutron star mergers and their beta-decay heating produces a visible early kilonova precursor for mass fractions above ~0.05.
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The First Infrared Portrait of A Solar-Like Host Star with Debris Disk: Pioneering High-Resolution H- and K-Band Spectroscopy of HD115617 with Comparative Optical Spectrum Analysis
The first NIR high-resolution spectroscopy of solar analog HD115617 shows a 250 K temperature discrepancy with optical data but confirms solar composition, main-sequence status, and no chemical signature of planetary formation.
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Constraints on the $^{12}$C$(\alpha, \gamma)^{16}$O and $^{16}$O+$^{16}$O Reaction Rates from Binary Black Holes Detected via Gravitational Wave Signals
Stellar models show that the 12C(alpha,gamma)16O rate uncertainty moves the black hole mass gap, constraining its S300 to 137.6-263.4 keV barn when matched to the observed gap from gravitational waves.
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Toward a Comprehensive Grid of Cepheid Models with MESA. IV. Modest Effects of Rotation on Blue Loops
Rotation produces only modest changes to blue loop luminosity and extent in MESA Cepheid models and cannot fix the mass discrepancy without substantial main-sequence overshooting.
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Type Ib supernovae are bluer than Type Ic supernovae
Type Ib supernovae are systematically bluer at optical peak than Type Ic supernovae, suggesting their progenitors contain more helium.
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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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Constraining the model-based uncertainties of asteroseismic magnetic field measurements in red giants
MESA grids show global magnetic sensitivity in red giants depends on mass and metallicity and can be recovered to 10% uncertainty with accurate spectroscopic metallicity.
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Simulations of Interacting Binary Systems -- Pathways to Radio Bright GRB Progenitors
Binary evolution simulations identify short (20-500 days) and long (2000-4000 days) orbital period ranges where massive star-black hole systems retain enough angular momentum for GRB jet production with negligible mass loss.