On the Prospects for Detection and Identification of Low-Frequency Oscillation Modes in Rotating B Type Stars

• Autorzy: Daszyńska-Daszkiewicz J. , Dziembowski W. A. , Pamyatnykh A. A.
• Języki publikacji: EN

Abstrakty

EN

We study how rotation affects observable amplitudes of high-order g- and mixed r/g-modes and examine prospects for their detection and identification. Our formalism, which is described in some detail, relies on a nonadiabatic generalization of the traditional approximation. Numerical results are presented for a number of unstable modes in a model of SPB star, at rotation rates up to 250 km/s. It is shown that rotation has a large effect on mode visibility in light and in mean radial velocity variations. In most cases, fast rotation impairs mode detectability of g-modes in light variation, as Townsend (2003b) has already noted, but it helps detection in radial velocity variation. The mixed modes, which exist only at sufficiently fast rotation, are also more easily seen in radial velocity. The amplitude ratios and phase differences are strongly dependent on the aspect, the rotational velocity and on the mode. The latter dependence is essential for mode identification.

Słowa kluczowe

EN

Stars: oscillations; Stars: emission-line; Stars:Be; Stars: rotation

• Wydawca: Copernicus Foundation for Polish Astronomy
• Czasopismo: Acta Astronomica
• Rocznik: 2007
• Tom: Vol. 57, No. 1
• Strony: 11--32
• Opis fizyczny: Bibliogr. 19 poz., rys., wykr.

Twórcy

autor

Daszyńska-Daszkiewicz J.

• Instytut Astronomiczny, Uniwersytet Wrocławski. ul. Kopernika 11, Poland

autor

Dziembowski W. A.

• Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warsaw, Poland
• Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland

autor

Pamyatnykh A. A.

• Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland
• Institute of Astronomy, Pyatnitskaya Str.48, 109017 Moscow, Russia

Bibliografia

• Baade, D. 1982, Astron. Astrophys., 10, 65.
• Balona, L. 1995, MNRAS, 306, 407.
• Bildsten, L., Ushomirsky, G., and Cutler, C. 1996, Astrophys. J., 460, 827.
• Castelli, F., and Kurucz, R.L. 2004, astro-ph/0405087 (http://kurucz.harvard.edu).
• Claret, A. 2000, Astron. Astrophys., 363, 1081.
• Daszyńska-Daszkiewicz, J., Dziembowski, W.A., and Pamyatnykh, A.A. 2003, Astron. Astrophys., 407, 999.
• Daszyńska-Daszkiewicz, J., Dziembowski, W.A., and Pamyatnykh, A.A. 2005, Astron. Astrophys., 441, 641.
• Dziembowski, W.A., Daszyńska-Daszkiewicz, J., and Pamyatnykh, A.A. 2007, MNRAS, 374, 248.
• Jerzykiewicz, M., et al. 2005, MNRAS, 360, 619.
• Lee, U. 2006, MNRAS, 365, 677.
• Lee, U., and Saio, H. 1997, Astrophys. J., 491, 839.
• Savonije, G.J. 2005, Astron. Astrophys., 443, 557.
• Saio, H., et al. 2007, Astrophys. J., 654, 544.
• Townsend, R.H.D. 2003a, MNRAS, 340, 1020.
• Townsend, R.H.D. 2003b, MNRAS, 343, 125.
• Townsend, R.H.D. 2005a, MNRAS, 360, 465.
• Townsend, R.H.D. 2005b, MNRAS, 364, 573.
• Walker, G.A.H., et al. 2005a, Astrophys. J. Letters, 623, L145.
• Walker, G.A.H., et al. 2005b, Astrophys. J. Letters, 635, L77.