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The pulsation modes of the pre-white dwarf PG 1159-035 | | J. E. S. Costa
; S. O. Kepler
; D. E. Winget
; M. S. O'Brien
; S. D. Kawaler
; A. F. M. Costa
; O. Giovannini
; A. Kanaan
; A. S. Mukadam
; F. Mullally
; A. Nitta
; J. L. Provençal
; H. Shipman
; M. A. Wood
; T. J. Ahrens
; A. Grauer
; M. Kilic
; P. A. Bradley
; K. Sekiguchi
; R. Crowe
; X. J. Jiang
; D. Sullivan
; T. Sullivan
; R. Rosen
; J. C. Clemens
; R. Janulis
; D. O'Donoghue
; W. Ogloza
; A. Baran
; R. Silvotti
; S. Marinoni
; G. Vauclair
; N. Dolez
; M. Chevreton
; S. Dreizler
; S. Schuh
; J. Deetjen
; T. Nagel
; J.-E. Solheim
; J. M. Gonzalez Perez
; A. Ulla
; Martin Barstow
; M. Burleigh
; S. Good
; T.S. Metcalfe
; S.-L. Kim
; H. Lee
; A. Sergeev
; M.C. Akan
; Ö. Çakirli
; M. Paparo
; G. Viraghalmy
; B. N. Ashoka
; G. Handler
; Özlem Hürkal
; F. Johannessen
; S. J. Kleinman
; R. Kalytis
; J. Krzesinski
; | | Date: |
14 Nov 2007 | | Abstract: | PG 1159-035, a pre-white dwarf with T_eff=140,000 K, is the prototype of both
two classes: the PG1159 spectroscopic class and the DOV pulsating class.
Previous studies of PG 1159-035 photometric data obtained with the Whole Earth
Telescope (WET) showed a rich frequency spectrum allowing the identification of
122 pulsation modes. In this work, we used all available WET photometric data
from 1983, 1985, 1989, 1993 and 2002 to identify the pulsation periods and
identified 76 additional pulsation modes, increasing to 198 the number of known
pulsation modes in PG 1159-035, the largest number of modes detected in any
star besides the Sun. From the period spacing we estimated a mass M = 0.59 +/-
0.02 solar masses for PG 1159-035, with the uncertainty dominated by the
models, not the observation. Deviations in the regular period spacing suggest
that some of the pulsation modes are trapped, even though the star is a
pre-white dwarf and the gravitational settling is ongoing. The position of the
transition zone that causes the mode trapping was calculated at r_c = 0.83 +/-
0.05 stellar radius. From the multiplet splitting, we calculated the rotational
period P_rot = 1.3920 +/- 0.0008 days and an upper limit for the magnetic
field, B < 2000 G. The total power of the pulsation modes at the stellar
surface changed less than 30% for l=1 modes and less than 50% for l=2 modes. We
find no evidence of linear combinations between the 198 pulsation mode
frequencies. PG 1159-035 models have not significative convection zones,
supporting the hypothesis that nonlinearity arises in the convection zones in
cooler pulsating white dwarf stars. | | Source: | arXiv, 0711.2244 | | Services: | Forum | Review | PDF | Favorites | |
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