Issue |
A&A
Volume 490, Number 3, November II 2008
|
|
---|---|---|
Page(s) | 1109 - 1120 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:200809890 | |
Published online | 17 September 2008 |
The detection of the rich p-mode spectrum and asteroseismology of Przybylski's star *
1
Astrophysical Research Center for the Structure and Evolution of the Cosmos, Sejong University, Seoul 143-747, Korea e-mail: davidm@sejong.ac.kr
2
Astronomical Observatory, Odessa National University, Shevchenko Park, Odessa, 65014, Ukraine
3
Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778, Tautenburg, Germany e-mail: artie@tls-tautenburg.de
4
Astronomical Institute, School of Science, Tohoku University, Sendai 980-8578, Japan e-mail: saio@astr.tohoku.ac.jp
5
Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT, Australia e-mail: rshobb@gmail.com
Received:
2
April
2008
Accepted:
23
August
2008
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
–2
modes, having a large spacing of
Hz. We calculated the nonadiabatic frequencies of
axisymmetric high-order p-modes for main-sequence models with dipole
magnetic fields of two chemical compositions
and
. The former composition provided the best
fit model and yielded stellar parameters of mass,
,
age = (1.5 ± 0.1)
109 yr,
effective temperature
, luminosity
, surface gravity
, and polar magnetic field strength,
Bp =
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.
Key words: stars: chemically peculiar / stars: oscillations / stars: individual: HD 101065
© ESO, 2008
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