Test upload SPB stars

Description

Abstract (English)

Context.

Slowly pulsating B (SPB) stars display multi-periodic variability in the gravito-inertial mode regime with indications of non-linear resonances between modes. Several have undergone asteroseismic modeling in the past few years to infer their internal properties, but only in a linear setting. These stars rotate fast, so that rotation is typically included in the modeling by means of the traditional approximation of rotation (TAR).

Aims.

We aim to extend the set of tools available for asteroseismology, by describing time-independent (stationary) resonant non-linear coupling among three gravito-inertial modes within the TAR. Such coupling offers the opportunity to use mode amplitude ratios in the asteroseismic modeling process, instead of only relying on frequencies of linear eigenmodes, as has been done so far.

Methods.

Following observational detections, we derive expressions for the resonant stationary non-linear coupling between three gravito-inertial modes in rotating stars. We assess selection rules and stability domains for stationary solutions. We also predict non-linear frequencies and amplitude ratio observables that can be compared with their observed counterparts.

Results.

The non-linear frequency shifts of stationary couplings are negligible compared to typical frequency errors derived from observations. The theoretically predicted amplitude ratios of combination frequencies match with some of their observational counterparts in the SPB targets. Other, unexplained observed ratios could be linked to other saturation mechanisms, to interactions between different modes, or to different opacity gradients in the driving zone.

Conclusions.

For the purpose of asteroseismic modeling, our non-linear mode coupling formalism can explain some of the stationary amplitude ratios of observed resonant mode couplings in single SPB stars monitored during 4 years by the Kepler space telescope.

Technical info (English)

Available AESolver materials

Inlists

The zipped archive inlists_aesolver.zip contains the different inlists used to generate the data products (i.e., the mode coupling models). These inlists are formatted as .toml files (see https://toml.io/en/ for additional information on this file format).

The names of the these `toml inlists' reflect the information contained within the final data products of the 'runs' they will initiate, and can be deconstructed in the following way: 

model_x_y_jvb_2023.toml  (or model_x_jvb_2023.toml)

where 'x' refers to the main model number and 'y' is an optional additional number used to denote sub-models.

The main model numbers can be mapped in the following way to the models used in Tables 2, 3, 4, 5 and 6 of  Van Beeck et al. (2024)(ArXiv link):

 The (optional) additional numbers were used to distinguish between sub-models when linearly excited \((k,m) = (0,1)\) were encountered when forming potential mode triads (see the discussion in Section 4 of Van Beeck et al. (2024)). Prior to the generation of the figures in Van Beeck et al. (2024) and the generation of the data within the tables of that paper, such sub-models are stitched automatically using the functionality of the AESolver code (see the documentation website https://jvb11.github.io/AESolver/ for more information on how to perform such automatic stitching.)

Data products

The zipped archive aesolver_output_files.zip contains the data products generated using the inlists described in the previous sub-section.

Their names match those of the inlists. When generating the data for the tables of, and the figures in Van Beeck et al. (2024) any sub-models are automatically stitched.

An overview of the contents of these data products can be found on the documentation website (https://jvb11.github.io/AESolver/).

Technical info (English)

Available GYRE materials

Inlists

Data products

Technical info (English)

Available MESA materials

Inlists

Data products