Porto Oscillation Code (POSC)

Abstract

The Porto Oscillation Code (POSC) has been developed in 1995 and improved over the years, with the main goal of calculating linear adiabatic oscillations for models of solar-type stars. It has also been used to estimate the frequencies and eigenfunctions of stars from the pre-main sequence up to the sub-giant phase, having a mass between 0.8 and 4 solar masses. The code solves the linearised perturbation equations of adiabatic pulsations for an equilibrium model using a second order numerical integration method. The possibility of using Richardson extrapolation is implemented. Several options for the surface boundary condition can be used. In this work we briefly review the key ingredients of the calculations, namely the equations, the numerical scheme and the output.

Accepted for publication in Astrophysics and Space Sciences

References in corpus (8)

• ADIPLS -- the Aarhus adiabatic oscillation package
• ASTEC -- the Aarhus STellar Evolution Code
• Seismic analysis of the second ionization region of helium in the Sun: I. Sensitivity study and methodology
• The CoRoT Evolution and Seismic Tools Activity: Goals and Tasks
• Inter-comparison of the g-, f- and p-modes calculated using different oscillation codes for a given stellar model
• Grids of stellar evolution models for asteroseismology (CESAM + POSC)
• A theoretical approach for the interpretation of pulsating PMS intermediate-mass stars
• Report on the CoRoT Evolution and Seismic Tools Activity

Cited by in corpus (6)

• Radius determination of solar-type stars using asteroseismology: What to expect from the Kepler mission
• Asteroseismology of solar-type stars
• The CoRoT Evolution and Seismic Tools Activity: Goals and Tasks
• Stellar model fits and inversions
• New scaling relations from MESA models for mass and radius of subgiant stars: application to Kepler targets
• On the possibility of using seismic probes to study the core composition in pulsating white dwarfs