RUBIS: a simple tool for calculating the centrifugal deformation of stars and planets
arXiv:2303.08077 · doi:10.1051/0004-6361/202346403
Abstract
We present RUBIS (Rotation code Using Barotropy conservation over Isopotential Surfaces), a fully Python-based centrifugal deformation program available at \url{https://github.com/pierrehoudayer/RUBIS}. The code has been designed to calculate the centrifugal deformation of stars and planets resulting from a given cylindrical rotation profile, starting from a spherically symmetric non-rotating model. The underlying assumption in RUBIS is that the relationship between density and pressure is preserved during the deformation process. This leads to many procedural simplifications. For instance, RUBIS only needs to solve Poisson' equation, either in spheroidal or spherical coordinates depending on whether the 1D model has discontinuities or not. We present the benefits of using RUBIS to deform polytropic models and more complex barotropic structures, thus providing, to a certain extent, insights into baroclinic models. The resulting structures can be used for a wide range of applications, including the seismic study of models. Finally, we illustrate how RUBIS is beneficial specifically in the analysis of Jupiter's gravitational moments, thanks to its ability to handle discontinuous models while retaining a high accuracy compared to current methods.
References in corpus (14)
- Comparing Jupiter interior structure models to Juno gravity measurements and the role of a dilute core
- Imaging the Surface of Altair
- Rotational mixing in low-mass stars II. Self-consistent models of Pop II RGB stars
- Acoustic oscillations of rapidly rotating polytropic stars. II. Effects of the Coriolis and centrifugal accelerations
- Saturn Ring Seismology: Evidence for Stable Stratification in the Deep Interior of Saturn
- Acoustic oscillations in rapidly rotating polytropic stars I. Effects of the centrifugal distortion
- Imaging and Modeling Rapidly Rotating Stars: Alpha Cephei and Alpha Ophiuchi
- Gravity modes in rapidly rotating stars. Limits of perturbative methods
- On the Structure and Properties of Differentially Rotating Main-Sequence Stars in the 1-2 M_sun Range
- A realistic two-dimensional model of Altair
- Pulsations of rapidly rotating stars: II. Realistic modelling for intermediate-mass stars
- Regular Oscillation Sub-spectrum of Rapidly Rotating Stars
- Oscillations of 2D ESTER models. I. The adiabatic case
- A complete study of the precision of the concentric MacLaurin spheroid method to calculate Jupiter's gravitational moments