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.
Title resolution pending
17 Pith papers cite this work. Polarity classification is still indexing.
17
Pith papers citing it
representative citing papers
Type Ib supernovae are systematically bluer than Type Ic supernovae in optical colors, likely due to helium-rich versus helium-poor progenitors.
Self-gravitating disks heated by stars reach a universal optical effective temperature of 4000-4500 K independent of accretion rate, black hole mass, and viscosity, explaining Little Red Dots.
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.
DSEE is a flow-based emulator that generates stellar evolution tracks and isochrones as probabilistic outputs from a single model trained on millions of simulations, enabling fast interpolation and uncertainty-aware analyses.
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.
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.
NGC 6791 has an age of 8.46 ± 0.66 Gyr, [Fe/H] = +0.280 ± 0.079, and other parameters that favor an inner-Galaxy origin followed by outward migration.
Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.
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.
MESA grid models of Procyon A and B give a system age of 2.23 Gyr, white dwarf cooling age of 1.20 Gyr, and map the progenitor to the 1.9-2.6 solar mass range with higher core overshoot than standard.
Asteroseismic fits to g-dominated mixed modes in four red giants suggest convective overshooting rises with mass and yield a core rotation rate of 0.7409 μHz for KIC 11968334.
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.
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
-
Constructing Earth Formation History Using Deep Mantle Noble Gas Reservoirs
Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.