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The Impact of Stellar Rotation on the Frequency Modes of V1790 Ori

Sun, Xiaoya; García Hernández, Antonio; Zuo, Zhaoyu

Publisher
Zenodo
DOI
10.5281/zenodo.17249553
Repository
zenodo.org
Language
en

Abstract

In recent years, with the abundance of high-precision observational data provided by space telescopes, δ Scuti stars exhibit complex and rich frequency spectra, making it possible to identify regular frequency patterns that can help to probe their internal structures. Current studies mainly analyze these frequencies by investigating the relationship between large separations and low-order modes (García Hernández et al. 2015,2017), as well as mode identification in echelle diagrams (Bedding et al. 2020). However, most of these studies neglect the effects of stellar rotation. This study aims to explore the impact of rotation on the frequencies of V179_Ori, mainly in the computation of the theoretical modes. We computed stellar equilibrium models including rotation using the MESA code. Pulsation frequencies were computed using GYRE (with first-order rotational corrections) and FILOU (with second-order rotational corrections). By analyzing the distribution of frequencies in the echelle diagrams under different treatments of rotation, we identified some splitting modes. Additionally, we have investigated the impact of mesh resolution on the accuracy of modes by comparing models with different numbers of mesh points (~800 vs ~4000), following the prescriptions of the ESTA/CoRoT exercises (Moya et al., 2008; and Li & Joyce, 2025).

Full text

. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . The Impact of Stellar Rotation on the Frequency Modes of V179 Ori Xiaoya Sun1,2, Zhaoyu Zuo1, Antonio García Hernández2 1Xi’an Jiaotong University, 2University of Granada, [email protected] Objectives Methodology Results GYRE FILOU 0 20 40 60 80 Periodicity [ Hz] 0.0 0.2 0.4 0.6 0.8 1.0 Normalised Power 0 20 40 60 80 Periodicity [ Hz] 0.2 0.4 0.6 0.8 1.0 Normalised Power 0 20 40 60 80 Periodicity [ Hz] 0.0 0.2 0.4 0.6 0.8 1.0 Normalised Power 0 20 40 60 80 100 mod ~ 87 Hz 0 200 400 600 800 1000 Mesh point ~ 800 M = 1.54 M , R = 1.41 R , Z = 0.01, T eff = 7944K v rot = 69.9km/s, = 85.1 Hz, log ( L / L ) = 0.85 0 20 40 60 80 Periodicity [ Hz] 0.0 0.2 0.4 0.6 0.8 1.0 Normalised Power 0 20 40 60 80 Periodicity [ Hz] 0.2 0.4 0.6 0.8 1.0 Normalised Power 0 20 40 60 80 Periodicity [ Hz] 0.0 0.2 0.4 0.6 0.8 1.0 Normalised Power 0 20 40 60 80 100 mod ~ 87 Hz 0 200 400 600 800 1000 Frequency [ Hz] M = 1.54 M , R = 1.40 R , Z = 0.01, T eff = 8060K v rot = 69.6km/s, = 86.2 Hz, log ( L / L ) = 0.85 0 20 40 60 80 Periodicity [ Hz] 0.0 0.2 0.4 0.6 0.8 1.0 Normalised Power 0 20 40 60 80 Periodicity [ Hz] 0.2 0.4 0.6 0.8 1.0 Normalised Power 0 20 40 60 80 Periodicity [ Hz] 0.0 0.2 0.4 0.6 0.8 1.0 Normalised Power 0 20 40 60 80 100 mod ~ 87 Hz 0 200 400 600 800 1000 Mesh point ~ 4000 M = 1.58 M , R = 1.42 R , Z = 0.01, T eff = 8120K v rot = 69.9km/s, = 85.0 Hz, log ( L / L ) = 0.90 0 20 40 60 80 Periodicity [ Hz] 0.0 0.2 0.4 0.6 0.8 1.0 Normalised Power 0 20 40 60 80 Periodicity [ Hz] 0.2 0.4 0.6 0.8 1.0 Normalised Power 0 20 40 60 80 Periodicity [ Hz] 0.0 0.2 0.4 0.6 0.8 1.0 Normalised Power 0 20 40 60 80 100 mod ~ 87 Hz 0 200 400 600 800 1000 Frequency [ Hz] M = 1.61 M , R = 1.42 R , Z = 0.01, T eff = 8283K v rot = 69.6km/s, = 86.7 Hz, log ( L / L ) = 0.92 References & Funding TODOS 9th TESS/16th Kepler Asteroseismic Science Consortium Workshop July 7-11, 2025