On the origin of variability in α Cygni variable ε Ori (HD 37128) using TESS observations and modelling

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ID: 313734
2026
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Abstract
Abstract ε Ori (HD 37128) is an α Cygni variable characterized by irregular and small amplitude variations. From TESS observations, we find the presence of stochastic low-frequency variability in this star. We have constructed a sequence of models for this star in the mass range of 30 to 70 M⊙, using recently derived values of luminosity (log (L/L⊙) = 5.92) and effective temperature. In these considered models, both radial and non-radial linear stability analyses have been performed. Low-order radial modes are excited in models having mass below 62 M⊙. These radially excited modes have periods ranging from 6.8 days for the fundamental mode to a few hours for higher-order modes. Similar to the case of radial modes, several non-radial modes are found to be unstable in models having higher luminosity-to-mass ratios. Linear stability analysis for the case of l = 2 and l = 4 reveals the presence of a strongly unstable mode in models having a mass below 40 M⊙. This mode is found to be unstable in all the considered models and the strength of the instability varies as a function of harmonic degree. The non-adiabatic reversible approximation reveals that the origin of instabilities associated with the low-order modes is indeed linked with strange modes. To find out the consequence of radial instabilities, non-linear numerical simulations have been performed in selected models of ε Ori. In the non-linear regime, these instabilities lead to the envelope inflation, finite amplitude regular and irregular pulsations consistent with an α Cygni variable.
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Authors Subharthi Dasgupta, Sugyan Parida, Abhay Pratap Yadav, W. Glatzel, M. Kraus
Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag895
URL
https://doi.org/10.1093/mnras/stag895
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