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Clemens, Gabriele; Reinfeldt, Alexander; Rüter, Telse

doi:10.5771/9783748901785-407

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“…A best-fitting model is selected for each star by selecting a minimal value of χ. The two DAV stars have short-period modes observed, as shown in Table 2, and therefore they should have hot effective temperatures (Clemens 1993, Mukadam et al 2006. The corresponding two best-fitting models are really hot DAV star models, with T eff = 11900 K for G117-B1A and T eff = 12650 K for R548.…”

Section: Discussionmentioning

confidence: 94%

The rate of period change in DAV stars

Chen

et al. 2017

Res. Astron. Astrophys.

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Grids of DAV star models are evolved by WDEC, taking the element diffusion effect into account. The grid parameters are hydrogen mass log(M H /M * ), helium mass log(M He /M * ), stellar mass M * , and effective temperature T eff for DAV stars. The core compositions are from white dwarf models evolved by MESA. Therefore, those DAV star models evolved by WDEC have historically viable core compositions. Based on those DAV star models, we studied the rate of period change (Ṗ (k)) for different values of H, He, M * , and T eff . The results are consistent with previous work. Two DAV stars G117-B15A and R548 have been observed around forty years. The rates of period change of two largeamplitude modes were obtained through O-C method. We did asteroseismological study on the two DAV stars and then obtained a best-fitting model for each star. Based on the two best-fitting models, the mode identifications (l, k) of the observed modes for G117-B15A and R548 are consistent with previous work. Both the observed modes and the observeḋ P s can be fitted by calculated ones. The results indicate that our method of evolving DAV star models is feasible.

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Section: Discussionmentioning

confidence: 94%

The rate of period change in DAV stars

Chen

et al. 2017

Res. Astron. Astrophys.

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Cited by 1 publication

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The rate of period change in DAV stars

The rate of period change in DAV stars

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