The detection of the rich p-mode spectrum and asteroseismology of Przybylski's star

Details The detection of the rich p-mode spectrum and asteroseismology of Przybylski's star The detection of the rich p-mode spectrum and asteroseismology of Przybylski's star

Nov 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008a%26a...490.1109m&link_type=abstract

Astronomy and Astrophysics, Volume 490, Issue 3, 2008, pp.1109-1120

Astronomy and Astrophysics

Astrophysics

9

Stars: Chemically Peculiar, Stars: Oscillations, Stars: Individual: Hd 101065

Scientific paper

Aims: We investigate the oscillation spectrum of the most chemically-peculiar star in the sky, the rapidly-oscillating magnetic (roAp) star HD 101065. Methods: High-precision radial velocity (RV) measurements, spanning four consecutive nights on 3-6 March, 2004, were obtained with the HARPS echelle-spectrometer at the ESO 3.6-m telescope, and photometric data were acquired during 6 nights of observations at the 24-inch telescope of Siding Spring Observatory. The RVs were measured using all spectral lines in the wavelength range 4400-5100 Å. Results: We detected a rich spectrum of oscillation modes with semi-amplitudes ranging between 217 m s-1 and 1.6 m s-1. These belong to the complete spectrum of high-order, low ℓ = 0-2 modes, having a large spacing of overlineΔ ν = 64.07 ± 0.9 μHz. We calculated the nonadiabatic frequencies of axisymmetric high-order p-modes for main-sequence models with dipole magnetic fields of two chemical compositions (X,Z)= (0.7,0.02) and (X,Z) = (0.695,0.025). The former composition provided the best fit model and yielded stellar parameters of mass, M=1.525 ± 0.025 M_&sun;, age = (1.5 ± 0.1) × 109 yr, effective temperature log T_e=3.821 ± 0.006, luminosity log L/L&sun;= 0.797 ± 0.026, surface gravity log g=4.06 ±0.04, and polar magnetic field strength, Bp = 8.7± 0.3 kG. We are able to identify the modes of all detected oscillation frequencies. The photometric U and B light curves have maxima that precede the RV maximum by 0.16-0.19 in phase.
Based on observations made on the 3.6 m Telescope at La Silla of the European Southern Observatory under program 072.D-0286.

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