Apsidal motion and non-radial pulsations in psi 2 Ori

Details Apsidal motion and non-radial pulsations in psi 2 Ori Apsidal motion and non-radial pulsations in psi 2 Ori

Oct 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...377..104t&link_type=abstract

Astronomy and Astrophysics, v.377, p.104-112 (2001)

Astronomy and Astrophysics

Astrophysics

13

Stars: Early-Type, Stars: Oscillations, Line: Profiles, Binaries: Close, Binaries: Spectroscopic, Stars: Individual: Psi 2</Sup&Gt, Ori

Scientific paper

We present a time series of high-resolution echelle spectra of the double-lined close binary psi 2 Ori. The spectra sample the wavelength region of 3800-6800 Å. In the absorption lines of the early-B type primary we find clear evidence for non-radial pulsations with intermediate values of the modal degree l. Using a cross-correlation technique we derive the radial velocity of both components. We compare our orbital solution with those reported in the literature to derive the apsidal motion period in this system: 47.5 +/- 0.7 year. We analyse the absorption line profiles of the primary using Fourier techniques to derive apparent pulsation periods and l values of two detected modes with apparent frequencies f_1=10.48 c/d and f_2=10.73 c/d. We discuss whether the non-radial pulsations in this star are internally excited or due to tidal forcing. Comparing the pulsation frequencies with those expected for tidal forcing and for internally excited modes, we tentatively conclude that these modes are probably due to internally excited beta Cephei pulsations. Based on observations made with the Isaac Newton Telescope operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.

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