Extended q-PED modeling provides first mass estimates for SMC Cepheids and new period-mass-radius and mass-luminosity relations while indicating binary interactions in several systems.
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Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation
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abstract
We update the capabilities of the open-knowledge software instrument Modules for Experiments in Stellar Astrophysics (MESA). RSP is a new functionality in MESAstar that models the non-linear radial stellar pulsations that characterize RR Lyrae, Cepheids, and other classes of variable stars. We significantly enhance numerical energy conservation capabilities, including during mass changes. For example, this enables calculations through the He flash that conserve energy to better than 0.001 %. To improve the modeling of rotating stars in MESA, we introduce a new approach to modifying the pressure and temperature equations of stellar structure, and a formulation of the projection effects of gravity darkening. A new scheme for tracking convective boundaries yields reliable values of the convective-core mass, and allows the natural emergence of adiabatic semiconvection regions during both core hydrogen- and helium-burning phases. We quantify the parallel performance of MESA on current generation multicore architectures and demonstrate improvements in the computational efficiency of radiative levitation. We report updates to the equation of state and nuclear reaction physics modules. We briefly discuss the current treatment of fallback in core-collapse supernova models and the thermodynamic evolution of supernova explosions. We close by discussing the new MESA Testhub software infrastructure to enhance source-code development.
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representative citing papers
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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.
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}.
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.
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.
New 2025 transit timing of HIP 41378 f shows a 7-hour early arrival consistent with TTVs; N-body modeling with TRADES refines ephemerides for planets d, e, and f.
Updated ab initio tidal models predict Earth survives the Sun's giant phases, but outcomes depend strongly on AGB mass-loss rates, with L2 Pup observations as proxy indicating survival while low rates lead to engulfment.
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.
Synthetic spectra show that observational biases cause dipole mode visibilities to be overestimated by up to 20 percent on the red-giant branch, while partial energy preservation under magnetic damping can produce both present and absent mixed-mode signatures.
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 helium flash produces a neutrino burst with a 1.7 MeV line detectable up to almost 3 pc in future facilities, but asteroseismology remains the practical probe for now.
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.
MESA models show residual hydrogen envelope mass sets effective temperature on the horizontal branch, with maximum values of 0.05-0.30 solar masses to avoid later thermally pulsing AGB evolution, plus explanations for blue hook stars and puffed-up pre-HB configurations.
New upper bounds on millicharged particles (masses 10-100 keV, charges down to 5e-13) from the AGB-to-HB star ratio in globular clusters, improving prior limits by up to two orders of magnitude.
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.
Magnetic wind braking can slow ssrAp stars like 33 Lib to rotation periods of 80 years or more according to MESA evolution models that include magnetic field and wind changes.
Observational analysis of HD210684 yields rotational period 5.02188 d, magnetic obliquity 77°, and main-sequence age ~1.45 Gyr from photometry, LSD magnetic measurements, and MESA/GYRE modeling.
Theoretical predictions for local BBH merger rates exceed observations by a factor >10 under conservative SFRD and metallicity assumptions, indicating need for revisions in stellar evolution.
A synthesis of observational data on red novae as stellar merger events, including outburst properties, progenitor diversity, and long-term remnants.
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