SIMBAD references

2006MNRAS.365..327H - Mon. Not. R. Astron. Soc., 365, 327-338 (2006/January-1)

Asteroseismology of the β Cephei star 12 (DD) Lacertae: photometric observations, pulsational frequency analysis and mode identification.

HANDLER G., JERZYKIEWICZ M., RODRIGUEZ E., UYTTERHOEVEN K., AMADO P.J., DOROKHOVA T.N., DOROKHOV N.I., PORETTI E., SAREYAN J.-P., PARRAO L., LORENZ D., ZSUFFA D., DRUMMOND R., DASZYNSKA-DASZKIEWICZ J., VERHOELST T., DE RIDDER J., ACKE B., BOURGE P.-O., MOVCHAN A.I., GARRIDO R., PAPARO M., SAHIN T., ANTOCI V., UDOVICHENKO S.N., CSORBA K., CROWE R., BERKEY B., STEWART S., TERRY D., MKRTICHIAN D.E. and AERTS C.

Abstract (from CDS):

We report a multisite photometric campaign for the β Cephei star 12 Lacertae. 750 h of high-quality differential photoelectric Strömgren, Johnson and Geneva time-series photometry were obtained with nine telescopes during 190 nights. Our frequency analysis results in the detection of 23 sinusoidal signals in the light curves. Ten of those correspond to independent pulsation modes, and the remainder are combination frequencies. We find some slow aperiodic variability such as that seemingly present in several β Cephei stars. We perform mode identification from our colour photometry, derive the spherical degree ℓ for the five strongest modes unambiguously and provide constraints on ℓ for the weaker modes. We find a mixture of modes of 0 ≤ℓ≤ 4. In particular, we prove that the previously suspected rotationally split triplet within the modes of 12 Lac consists of modes of different ℓ; their equal frequency splitting must thus be accidental.

One of the periodic signals we detected in the light curves is argued to be a linearly stable mode excited to visible amplitude by non-linear mode coupling via a 2:1 resonance. We also find a low-frequency signal in the light variations whose physical nature is unclear; it could be a parent or daughter mode resonantly coupled. The remaining combination frequencies are consistent with simple light-curve distortions.

The range of excited pulsation frequencies of 12 Lac may be sufficiently large that it cannot be reproduced by standard models. We suspect that the star has a larger metal abundance in the pulsational driving zone, a hypothesis also capable of explaining the presence of β Cephei stars in the Large Magellanic Cloud.

Journal keyword(s): techniques: photometric - stars: early-type - stars: individual: 12 (DD) Lacertae - stars: oscillations - stars: variables: other

Errata: erratum vol. 426, p. 2600 (2012)

Simbad objects: 13

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