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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13 Pith papers cite this work. Polarity classification is still indexing.
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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.
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.
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.
2D core-collapse supernova simulations of 15 solar-mass progenitors with varied multi-D initial structures show similar explosion dynamics, with no detectable impact from progenitor turbulence due to saturation by post-shock instabilities.
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.
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.
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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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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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.
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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.
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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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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.
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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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Impacts of Multidimensional Progenitor Perturbations on Core-Collapse Supernova Explosions
2D core-collapse supernova simulations of 15 solar-mass progenitors with varied multi-D initial structures show similar explosion dynamics, with no detectable impact from progenitor turbulence due to saturation by post-shock instabilities.
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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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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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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.