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Confirmation of Solar-Like Oscillations in η Bootis

  • H. Kjeldsen (a1), T.R. Bedding (a2), I.K. Baldry (a2), S. Frandsen (a3), H. Bruntt (a3), F. Grundahl (a3), K. Lang (a3), R.P. Butler (a4), D.A. Fischer (a5), G.W. Marcy (a5), A. Misch (a6) and S.S. Vogt (a6)...

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Kjeldsen et al. (1995) detected excess power in the GO subgiant η Boo from measurements of Balmer-line equivalent widths. The excess was at the expected level, and these authors were able to extract frequency separations and individual frequencies which agreed well with theoretical models (Christensen-Dalsgaard et al., 1995; Guenther & Demarque, 1996). A more detailed discussion of theoretical models for η Bootis was given by Di Mauro & Christensen-Dalsgaard (2001).

Kjeldsen et al. (1995) estimated the average amplitude of the strongest modes to be 7 times solar, corresponding to 1.6 m/s in velocity. 13 individual oscillation modes were identified consistent with a large frequency separation of 40.3 μHz. We note, however, that a search for velocity oscillations in this star by Brown et al. (1997) failed to detect a signal, setting limits at a level below that expected on the basis of the Kjeldsen et al. result.

In this paper we report further observations made in 1998. We observed this star in Balmer-line equivalent width with the 2.5-m Nordic Optical Telescope and in velocity with the 24-inch Lick CAT.

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References

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Brown, T.M., Kennelly, E.J., Korzennik, S.G., et al. 1997, ApJ, 475, 322
Christensen-Dalsgaard, J., Bedding, T.R., & Kjeldsen, H. 1995, ApJ, 443, L29
Di Mauro, M.P. & Christensen-Dalsgaard, J. 2001, in Proceedings of the SOHO 10/GONG 2000 Conference, ed. Wilson, A., SP-464, 373
Guenther, D.B. & Demarque, P. 1996, ApJ, 456, 798
Kjeldsen, H. & Bedding, T.R. 2001, in Proceedings of the SOHO 10/GONG 2000 Conference, ed. Wilson, A., SP-464, 361
Kjeldsen, H., Bedding, T.R., Viskum, M., & Frandsen, S. 1995, AJ, 109, 1313

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