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.
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Modules for Experiments in Stellar Astrophysics (MESA)
11 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
Stellar physics and evolution calculations enable a broad range of research in astrophysics. Modules for Experiments in Stellar Astrophysics (MESA) is a suite of open source libraries for a wide range of applications in computational stellar astrophysics. A newly designed 1-D stellar evolution module, MESA star, combines many of the numerical and physics modules for simulations of a wide range of stellar evolution scenarios ranging from very-low mass to massive stars, including advanced evolutionary phases. MESA star solves the fully coupled structure and composition equations simultaneously. It uses adaptive mesh refinement and sophisticated timestep controls, and supports shared memory parallelism based on OpenMP. Independently usable modules provide equation of state, opacity, nuclear reaction rates, and atmosphere boundary conditions. Each module is constructed as a separate Fortran 95 library with its own public interface. Examples include comparisons to other codes and show evolutionary tracks of very low mass stars, brown dwarfs, and gas giant planets; the complete evolution of a 1 Msun star from the pre-main sequence to a cooling white dwarf; the Solar sound speed profile; the evolution of intermediate mass stars through the thermal pulses on the He-shell burning AGB phase; the interior structure of slowly pulsating B Stars and Beta Cepheids; evolutionary tracks of massive stars from the pre-main sequence to the onset of core collapse; stars undergoing Roche lobe overflow; and accretion onto a neutron star. Instructions for downloading and installing MESA can be found on the project web site (http://mesa.sourceforge.net/).
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Gas giants form sub-snowline in binaries via dust traps at the tidal truncation radius, with observed planet semi-major axes following a_planet = 0.569 r_t (R²=0.94).
Hypercritical accretion onto neutron stars embedded in massive envelopes leads to rapid collapse into black holes rather than stable Thorne-Zytkow objects.
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}.
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.
Hot Jupiter occurrence in the Galactic halo is low at ~0.13% with no significant difference between in-situ and accreted populations, well below disk rates.
Revised supernova opacity modeling reopens the Turner window for hadronically coupled axions, enabling resonant absorption searches in NaI detectors for couplings |g_app| between 10^{-6.5} and 10^{-2}.
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.
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.
A synthesis of observational data on red novae as stellar merger events, including outburst properties, progenitor diversity, and long-term remnants.
citing papers explorer
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TESS Observations of Stochastic Low-frequency Variability in Extreme Helium Stars
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.
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Sub-Snowline Formation of Gas-Giant Planets in Binary Systems
Gas giants form sub-snowline in binaries via dust traps at the tidal truncation radius, with observed planet semi-major axes following a_planet = 0.569 r_t (R²=0.94).
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Hyperaccreting Neutron Stars inside Massive Envelopes: The Implausibility of Thorne-\.Zytkow Objects
Hypercritical accretion onto neutron stars embedded in massive envelopes leads to rapid collapse into black holes rather than stable Thorne-Zytkow objects.
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The Black Hole Mass Gap as a New Probe of Millicharged Particles
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}.
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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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Exoplanets in ancient stellar populations: occurrence constraints and hot-Jupiter candidates in the Galactic halo
Hot Jupiter occurrence in the Galactic halo is low at ~0.13% with no significant difference between in-situ and accreted populations, well below disk rates.
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Revisiting Turner Window Axions: The Untapped Potential of NaI Dark Matter Detectors
Revised supernova opacity modeling reopens the Turner window for hadronically coupled axions, enabling resonant absorption searches in NaI detectors for couplings |g_app| between 10^{-6.5} and 10^{-2}.
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Detection horizon for the neutrino burst from the stellar helium flash
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.
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Diagnosing the Properties and Evolutionary Fates of Black Hole and Wolf-Rayet X-ray Binaries as Potential Gravitational Wave Sources for the LIGO-Virgo-KAGRA Network
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.
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Modeling of the magnetic stellar wind braking of the ssrAp 33 Lib (HD137949)
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.
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Red novae, their progenitors, and remnants
A synthesis of observational data on red novae as stellar merger events, including outburst properties, progenitor diversity, and long-term remnants.