The Pulsation Modes Of The Pre-White Dwarf PG 1159-035

dc.contributor.utaustinauthorWinget, D.E.en_US
dc.contributor.utaustinauthorMullally, F.en_US
dc.creatorCosta, J. E. S.en_US
dc.creatorKepler, S. O.en_US
dc.creatorWinget, D. E.en_US
dc.creatorO'Brien, M. S.en_US
dc.creatorKawaler, S. D.en_US
dc.creatorCosta, A. F. M.en_US
dc.creatorGiovannini, O.en_US
dc.creatorKanaan, A.en_US
dc.creatorMukadam, A. S.en_US
dc.creatorMullally, F.en_US
dc.creatorNitta, A.en_US
dc.creatorProvencal, J. L.en_US
dc.creatorShipman, H.en_US
dc.creatorWood, M. A.en_US
dc.creatorAhrens, T. J.en_US
dc.creatorGrauer, A.en_US
dc.creatorKilic, M.en_US
dc.creatorBradley, P. A.en_US
dc.creatorSekiguchi, K.en_US
dc.creatorCrowe, R.en_US
dc.creatorJiang, X. J.en_US
dc.creatorSullivan, D.en_US
dc.creatorSullivan, T.en_US
dc.creatorRosen, R.en_US
dc.creatorClemens, J. Christopheren_US
dc.creatorJanulis, R.en_US
dc.creatorO'Donoghue, D.en_US
dc.creatorOgloza, W.en_US
dc.creatorBaran, A.en_US
dc.creatorSilvotti, R.en_US
dc.creatorMarinoni, S.en_US
dc.creatorVauclair, G.en_US
dc.creatorDolez, N.en_US
dc.creatorChevreton, M.en_US
dc.creatorDreizler, S.en_US
dc.creatorSchuh, S.en_US
dc.creatorDeetjen, J.en_US
dc.creatorNagel, T.en_US
dc.creatorSolheim, J. E.en_US
dc.creatorPerez, J. M. G.en_US
dc.creatorUlla, A.en_US
dc.creatorBarstow, M.en_US
dc.creatorBurleigh, M.en_US
dc.creatorGood, S.en_US
dc.creatorMetcalfe, T. S.en_US
dc.creatorKim, S. L.en_US
dc.creatorLee, H.en_US
dc.creatorSergeev, A.en_US
dc.creatorAkan, M. C.en_US
dc.creatorCakirli, O.en_US
dc.creatorPaparo, M.en_US
dc.creatorViraghalmy, G.en_US
dc.creatorAshoka, B. N.en_US
dc.creatorHandler, G.en_US
dc.creatorHurkal, O.en_US
dc.creatorJohannessen, F.en_US
dc.creatorKleinman, S. J.en_US
dc.creatorKalytis, R.en_US
dc.creatorKrzesinski, J.en_US
dc.creatorKlumpe, E.en_US
dc.creatorLarrison, J.en_US
dc.creatorLawrence, T.en_US
dc.creatorMeistas, E.en_US
dc.creatorMartinez, P.en_US
dc.creatorNather, R. E.en_US
dc.creatorFu, J. N.en_US
dc.creatorPakstiene, E.en_US
dc.creatorRosen, R.en_US
dc.creatorRomero-Colmenero, E.en_US
dc.creatorRiddle, R.en_US
dc.creatorSeetha, S.en_US
dc.creatorSilvestri, N. M.en_US
dc.creatorVuckovic, M.en_US
dc.creatorWarner, B.en_US
dc.creatorZolao, S.en_US
dc.creatorAlthaus, L. G.en_US
dc.creatorCorsico, A. H.en_US
dc.creatorMontgomery, M. H.en_US
dc.description.abstractContext. PG 1159-035, a pre-white dwarf with T-eff similar or equal to 140000 K, is the prototype of both two classes: the PG 1159 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. Analyzing the periods of pulsation, it is possible to measure the stellar mass, the rotational period and the inclination of the rotation axis, to estimate an upper limit for the magnetic field, and even to obtain information about the inner stratification of the star. Aims. We have three principal aims: to increase the number of detected and identified pulsation modes in PG 1159-035, study trapping of the star's pulsation modes, and to improve or constrain the determination of stellar parameters. Methods. We used all available WET photometric data from 1983, 1985, 1989, 1993 and 2002 to identify the pulsation periods. Results. We 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/M-circle dot = 0.59 +/- 0.02 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)/R-*, = 0.83 +/- 0.05. 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.en_US
dc.description.sponsorshipNSF AST-0507639en_US
dc.identifier.citationCosta, Jose Eduardo da Silveira, Souza Oliveira Kepler, Donald Earl Winget, M. Sean O'Brien, Steven D. Kawaler, Alex Fabiano Murillo da Costa, O. Giovannini et al. >The pulsation modes of the pre-white dwarf PG 1159-035.> Astronomy & Astrophysics, Vol. 477, No. 2 (Jan., 2008): pp. 627-640.en_US
dc.relation.ispartofserialAstronomy & Astrophysicsen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectstars : oscillationsen_US
dc.subjectstars : individual : pg 1159-035en_US
dc.subjectstars :en_US
dc.subjectstars : white dwarfsen_US
dc.subjectzz-ceti starsen_US
dc.subjectwhole earth telescopeen_US
dc.subjectplanetary-nebula nucleien_US
dc.subjectevolutionary modelsen_US
dc.subjectgravity modesen_US
dc.subjectpg 1159-035en_US
dc.subjectastronomy & astrophysicsen_US
dc.titleThe Pulsation Modes Of The Pre-White Dwarf PG 1159-035en_US

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