Considering the full spectrum of linear unstable modes allows the turbulent diffusion coefficient in thermohaline convection to self-consistently interpolate between previously discrepant theoretical scalings.
Title resolution pending
5 Pith papers cite this work. Polarity classification is still indexing.
5
Pith papers citing it
citation-role summary
background 1
citation-polarity summary
fields
astro-ph.SR 5roles
background 1polarities
background 1representative citing papers
MIST provides a new publicly available grid of solar-scaled stellar isochrones and evolutionary tracks computed self-consistently with MESA from pre-main sequence through advanced stages for masses 0.1-300 solar masses and metallicities -2 to 0.5.
MESA Star has been substantially updated with new capabilities for low-mass giant planets, asteroseismology coupling, rotating star models, and uninterrupted massive star evolution to core collapse.
Rotating stellar models initialized with observed velocity distributions yield modestly lower initial mass estimates for SN II progenitors than non-rotating models, with an upper limit of 20.4 solar masses.
MESA gains simultaneous binary star evolution, large nuclear networks, implicit hydrodynamics, and GYRE pulsation coupling for better massive star and supernova modeling.
citing papers explorer
-
Unifying Transport Models of Thermohaline Convection in Stars
Considering the full spectrum of linear unstable modes allows the turbulent diffusion coefficient in thermohaline convection to self-consistently interpolate between previously discrepant theoretical scalings.
-
MESA Isochrones and Stellar Tracks (MIST). I: Solar-Scaled Models
MIST provides a new publicly available grid of solar-scaled stellar isochrones and evolutionary tracks computed self-consistently with MESA from pre-main sequence through advanced stages for masses 0.1-300 solar masses and metallicities -2 to 0.5.
-
Modules for Experiments in Stellar Astrophysics (MESA): Giant Planets, Oscillations, Rotation, and Massive Stars
MESA Star has been substantially updated with new capabilities for low-mass giant planets, asteroseismology coupling, rotating star models, and uninterrupted massive star evolution to core collapse.
-
Impact of stellar rotation on type II supernova progenitor masses from pre-explosion imaging
Rotating stellar models initialized with observed velocity distributions yield modestly lower initial mass estimates for SN II progenitors than non-rotating models, with an upper limit of 20.4 solar masses.
-
Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions
MESA gains simultaneous binary star evolution, large nuclear networks, implicit hydrodynamics, and GYRE pulsation coupling for better massive star and supernova modeling.