The YNEV stellar evolution and oscillation code

TL;DR

The paper introduces YNEV, a comprehensive stellar evolution and oscillation code capable of modeling low- and intermediate-mass stars with advanced physics and convection theories, providing detailed stellar structure and oscillation data.

Contribution

YNEV is a new stellar evolution and oscillation code that incorporates nonlocal turbulent convection and updated overshoot models, enabling detailed simulations from pre-main sequence to white dwarf stages.

Findings

Successfully modeled solar and stellar evolutionary tracks.

Compared different convection theories in stellar evolution.

Calculated adiabatic oscillation eigenfrequencies for various stellar models.

Abstract

We have developed a new stellar evolution and oscillation code YNEV, which calculates the structures and evolutions of stars, taking into account hydrogen and helium burning. A nonlocal turbulent convection theory and an updated overshoot mixing model are optional in this code. The YNEV code can evolve low- and intermediate-mass stars from pre-main sequence (PMS) to thermal pulsing asymptotic branch giant (TP-AGB) or white dwarf. The YNEV oscillation code calculates the eigenfrequencies and eigenfunctions of the adiabatic oscillations of given stellar structure. The input physics and the numerical scheme adopted in the code are introduced in this paper. The examples of solar models, stellar evolutionary tracks of low- and intermediate-mass stars with different convection theory (i.e., mixing-length theory (MLT) and the nonlocal turbulent convection theory), and stellar oscillations are shown.