TESS data show stochastic low-frequency variability dominates in most extreme helium stars, with characteristic timescales of 0.5-10 days correlating to stellar parameters and matching subsurface convection predictions.
hub
Title resolution pending
38 Pith papers cite this work, alongside 1,926 external citations. Polarity classification is still indexing.
38
Pith papers citing it
1,926
external citations · Crossref
abstract
We update the capabilities of the software instrument Modules for Experiments in Stellar Astrophysics (MESA) and enhance its ease of use and availability. Our new approach to locating convective boundaries is consistent with the physics of convection, and yields reliable values of the convective core mass during both hydrogen and helium burning phases. Stars with $M<8\,{\rm M_\odot}$ become white dwarfs and cool to the point where the electrons are degenerate and the ions are strongly coupled, a realm now available to study with MESA due to improved treatments of element diffusion, latent heat release, and blending of equations of state. Studies of the final fates of massive stars are extended in MESA by our addition of an approximate Riemann solver that captures shocks and conserves energy to high accuracy during dynamic epochs. We also introduce a 1D capability for modeling the effects of Rayleigh-Taylor instabilities that, in combination with the coupling to a public version of the STELLA radiation transfer instrument, creates new avenues for exploring Type II supernovae properties. These capabilities are exhibited with exploratory models of pair-instability supernova, pulsational pair-instability supernova, and the formation of stellar mass black holes. The applicability of MESA is now widened by the capability of importing multi-dimensional hydrodynamic models into MESA. We close by introducing software modules for handling floating point exceptions and stellar model optimization, and four new software tools -- MESAWeb, MESA-Docker, pyMESA, and mesastar.org -- to enhance MESA's education and research impact.
hub tools
citation-role summary
background 3
citation-polarity summary
authors
roles
background 3polarities
background 3representative citing papers
Blue straggler stars in old open clusters exhibit a Kraft break in rotation, with rapid rotators above the break and slow rotators below, indicating their envelopes behave like those of single stars.
A PSF-fitting pipeline extracts variability light curves for 91 SMC massive stars and finds that stochastic low-frequency variability morphology tracks HR-diagram position independently of metallicity.
A score-based diffusion generative model on deep infrared galaxy photometry yields a star formation rate density peaking at z=1.3 and shows distinct non-parametric star formation histories plus AGN activity peaking during the quenching transition of massive galaxies.
Type Ib supernovae are systematically bluer than Type Ic supernovae in optical colors, likely due to helium-rich versus helium-poor progenitors.
Two long period radio transients are detached white dwarf-M dwarf binaries with matching periods, massive cool crystallized white dwarfs, low inclinations, and an estimated population of 100-2000 such systems within 2 kpc.
Dynamic Time Warping with a shared warping path across parameters aligns binary stellar tracks for accurate interpolation while preserving physical relationships such as the Stefan-Boltzmann law.
Millicharged particles weaken pulsational pair-instability in massive stars, shifting the lower edge of the black hole mass gap upward and turning gravitational wave observations into a probe for particles with masses 35-200 keV and charges 10^{-10} to 10^{-9}.
Physics-based annual TSI reconstruction over three millennia yields a maximum difference of 1.04 W/m² in 50-year running means.
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.
Blue straggler stars in old open clusters predominantly appear near the terminal-age main sequence because mass transfer from asymptotic giant branch donors enriches their cores with helium.
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.
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.
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.
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.
Tertiary in EM Boo is A-F type with Teff=7000K; system distance ~300 pc indicates Gaia DR3 underestimates true distance due to multiplicity.
MESA grid models find HD 20794 is a 0.80 solar-mass star aged ~9 Gyr whose observed abundances match core-collapse supernova enrichment and are preserved over Gyr timescales.
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.
Eruptive mass loss in red supergiants increases linearly with metallicity, calibrated via by-eye fits to Local Group luminosity functions, preventing initial masses above about 20 solar masses from reaching the red supergiant phase.
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.
MESA binary evolution simulations with revised Bondi-Hoyle accretion efficiency and observational constraints yield lower BH mass upper limits for IC 10 X-1 and NGC 300 X-1 and predict Hubble-time BBH mergers for all three systems.
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.
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.