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Evolutionary Model and Oscillation Frequencies for alpha Ursae Majoris: A Comparison with Observations.

Guenther, Demarque, Buzasi

    The Astrophysical Journal
    |January 21, 2000
    PubMed
    Summary

    Stellar models indicate alpha Ursae Majoris A is a red giant with a mass of 4.0-4.5 solar masses. Its observed oscillations are likely low-order radial p-modes, consistent with theoretical predictions.

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    Area of Science:

    • * Astrophysics
    • * Stellar Astrophysics
    • * Asteroseismology

    Background:

    • * Low-amplitude oscillations of alpha Ursae Majoris A observed by Buzasi et al. using the WIRE satellite.
    • * Red giants are crucial for understanding stellar evolution and internal structure.

    Purpose of the Study:

    • * To derive physically consistent interior models for alpha Ursae Majoris A.
    • * To interpret the observed low-amplitude oscillations in the context of stellar models.

    Main Methods:

    • * Construction of a grid of stellar evolutionary tracks.
    • * Calculation of pulsation properties for stellar models.
    • * Comparison of model predictions with observational data from WIRE satellite.

    Main Results:

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    • * Models with masses between 4.0-4.5 M☉ and normal helium abundance match observations.
    • * Oscillations are best explained as low radial order (n=0, 1, 2) radial (l=0) p-mode oscillations.
    • * Higher frequencies may correspond to higher radial order p-modes.
    • * Nonradial modes (l=1, 2, 3) are densely packed and unlikely to be resolved.

    Conclusions:

    • * The mass range of 4.0-4.5 M☉ is consistent with both asteroseismic data and astrometric mass function.
    • * The observed oscillations of alpha Ursae Majoris A provide strong constraints on its internal structure and evolutionary state.
    • * Further observations may resolve higher-order modes and nonradial oscillations.