Santander-Martinez, Petra Maria

[["dc.bibliographiccitation.firstpage","627"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","640"],["dc.bibliographiccitation.volume","477"],["dc.contributor.author","Costa, J. E. S."],["dc.contributor.author","Kepler, S. O."],["dc.contributor.author","Winget, D. E."],["dc.contributor.author","O'Brien, M. S."],["dc.contributor.author","Kawaler, S. D."],["dc.contributor.author","Costa, A. F. M."],["dc.contributor.author","Giovannini, O."],["dc.contributor.author","Kanaan, A."],["dc.contributor.author","Mukadam, A. S."],["dc.contributor.author","Mullally, F."],["dc.contributor.author","Nitta, A."],["dc.contributor.author","Provençal, J. L."],["dc.contributor.author","Shipman, H."],["dc.contributor.author","Wood, M. A."],["dc.contributor.author","Ahrens, T. J."],["dc.contributor.author","Grauer, A."],["dc.contributor.author","Kilic, M."],["dc.contributor.author","Bradley, P. A."],["dc.contributor.author","Sekiguchi, K."],["dc.contributor.author","Crowe, R."],["dc.contributor.author","Jiang, X. J."],["dc.contributor.author","Sullivan, D."],["dc.contributor.author","Sullivan, T."],["dc.contributor.author","Rosen, R."],["dc.contributor.author","Clemens, J. C."],["dc.contributor.author","Janulis, R."],["dc.contributor.author","O'Donoghue, D."],["dc.contributor.author","Ogloza, W."],["dc.contributor.author","Baran, A."],["dc.contributor.author","Silvotti, R."],["dc.contributor.author","Marinoni, S."],["dc.contributor.author","Vauclair, G."],["dc.contributor.author","Dolez, N."],["dc.contributor.author","Chevreton, M."],["dc.contributor.author","Dreizler, S."],["dc.contributor.author","Schuh, S."],["dc.contributor.author","Deetjen, J."],["dc.contributor.author","Nagel, T."],["dc.contributor.author","Solheim, J.-E."],["dc.contributor.author","Gonzalez Perez, J. M."],["dc.contributor.author","Ulla, A."],["dc.contributor.author","Barstow, M."],["dc.contributor.author","Burleigh, M."],["dc.contributor.author","Good, S."],["dc.contributor.author","Metcalfe, T. S."],["dc.contributor.author","Kim, S.-L."],["dc.contributor.author","Lee, H."],["dc.contributor.author","Sergeev, A."],["dc.contributor.author","Akan, M. C."],["dc.contributor.author","Çakırlı, Ö."],["dc.contributor.author","Paparo, M."],["dc.contributor.author","Viraghalmy, G."],["dc.contributor.author","Ashoka, B. N."],["dc.contributor.author","Handler, G."],["dc.contributor.author","Hürkal, Ö."],["dc.contributor.author","Johannessen, F."],["dc.contributor.author","Kleinman, S. J."],["dc.contributor.author","Kalytis, R."],["dc.contributor.author","Krzesinski, J."],["dc.contributor.author","Klumpe, E."],["dc.contributor.author","Larrison, J."],["dc.contributor.author","Lawrence, T."],["dc.contributor.author","Meištas, E."],["dc.contributor.author","Martinez, P."],["dc.contributor.author","Nather, R. E."],["dc.contributor.author","Fu, J.-N."],["dc.contributor.author","Pakštienė, E."],["dc.contributor.author","Romero-Colmenero, E."],["dc.contributor.author","Riddle, R."],["dc.contributor.author","Seetha, S."],["dc.contributor.author","Silvestri, N. M."],["dc.contributor.author","Vučković, M."],["dc.contributor.author","Warner, B."],["dc.contributor.author","Zola, S."],["dc.contributor.author","Althaus, L. G."],["dc.contributor.author","Córsico, A. H."],["dc.contributor.author","Montgomery, M. H."],["dc.date.accessioned","2019-07-09T11:53:29Z"],["dc.date.available","2019-07-09T11:53:29Z"],["dc.date.issued","2008"],["dc.description.abstract","Context. PG 1159-035, a pre-white dwarf with Teff 140 000 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 = 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 rc/R = 0.83 ± 0.05. From the multiplet splitting, we calculated the rotational period Prot = 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 = 1 modes and less than 50% for = 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."],["dc.identifier.doi","10.1051/0004-6361:20053470"],["dc.identifier.fs","513378"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/7676"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60434"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["dc.relation.orgunit","Fakultät für Physik"],["dc.rights","Goescholar"],["dc.rights.access","openAccess"],["dc.rights.uri","https://goedoc.uni-goettingen.de/licenses"],["dc.title","The pulsation modes of the pre-white dwarf PG 1159-035"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","639"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","654"],["dc.bibliographiccitation.volume","401"],["dc.contributor.author","Kepler, S. O."],["dc.contributor.author","Nather, R. E."],["dc.contributor.author","Winget, D. E."],["dc.contributor.author","Nitta, A."],["dc.contributor.author","Kleinman, S. J."],["dc.contributor.author","Metcalfe, T."],["dc.contributor.author","Sekiguchi, K."],["dc.contributor.author","Xiaojun, Jiang"],["dc.contributor.author","Sullivan, D."],["dc.contributor.author","Sullivan, T."],["dc.contributor.author","Janulis, R."],["dc.contributor.author","Meistas, E."],["dc.contributor.author","Kalytis, R."],["dc.contributor.author","Krzesinski, J."],["dc.contributor.author","Ogloza, W."],["dc.contributor.author","Zola, S."],["dc.contributor.author","O'Donoghue, D."],["dc.contributor.author","Romero-Colmenero, E."],["dc.contributor.author","Martinez, P."],["dc.contributor.author","Dreizler, S."],["dc.contributor.author","Deetjen, J."],["dc.contributor.author","Nagel, T."],["dc.contributor.author","Schuh, S. L."],["dc.contributor.author","Vauclair, G."],["dc.contributor.author","Ning, Fu Jian"],["dc.contributor.author","Chevreton, M."],["dc.contributor.author","Solheim, J.-E."],["dc.contributor.author","Perez, J. M. Gonzalez"],["dc.contributor.author","Johannessen, F."],["dc.contributor.author","Kanaan, A."],["dc.contributor.author","Costa, J. E."],["dc.contributor.author","Murillo Costa, A. F."],["dc.contributor.author","Wood, M. A."],["dc.contributor.author","Silvestri, N."],["dc.contributor.author","Ahrens, T. J."],["dc.contributor.author","Jones, A. K."],["dc.contributor.author","Collins, A. E."],["dc.contributor.author","Boyer, M."],["dc.contributor.author","Shaw, J. S."],["dc.contributor.author","Mukadam, A."],["dc.contributor.author","Klumpe, E. W."],["dc.contributor.author","Larrison, J."],["dc.contributor.author","Kawaler, S."],["dc.contributor.author","Riddle, R."],["dc.contributor.author","Ulla, A."],["dc.contributor.author","Bradley, P."],["dc.date.accessioned","2019-07-09T11:53:31Z"],["dc.date.available","2019-07-09T11:53:31Z"],["dc.date.issued","2003"],["dc.description.abstract","We report 323 hours of nearly uninterrupted time series photometric observations of the DBV star GD 358 acquired with the Whole Earth Telescope (WET) during May 23rd to June 8th, 2000. We acquired more than 232 000 independent measurements. We also report on 48 hours of time-series photometric observations in Aug 1996. We detected the non-radial g-modes consistent with degree ` = 1 and radial order 8 to 20 and their linear combinations up to 6th order. We also detect, for the first time, a high amplitude ` = 2 mode, with a period of 796 s. In the 2000 WET data, the largest amplitude modes are similar to those detected with the WET observations of 1990 and 1994, but the highest combination order previously detected was 4th order. At one point during the 1996 observations, most of the pulsation energy was transferred into the radial order k = 8 mode, which displayed a sinusoidal pulse shape in spite of the large amplitude. The multiplet structure of the individual modes changes from year to year, and during the 2000 observations only the k = 9 mode displays clear normal triplet structure. Even though the pulsation amplitudes change on timescales of days and years, the eigenfrequencies remain essentially the same, showing the stellar structure is not changing on any dynamical timescale."],["dc.identifier.doi","10.1051/0004-6361:20030105"],["dc.identifier.fs","20311"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/7683"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60437"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["dc.relation.orgunit","Fakultät für Physik"],["dc.rights","Goescholar"],["dc.rights.access","openAccess"],["dc.rights.uri","https://goedoc.uni-goettingen.de/licenses"],["dc.title","The everchanging pulsating white dwarf GD358"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","219"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","224"],["dc.bibliographiccitation.volume","432"],["dc.contributor.author","Kanaan, A."],["dc.contributor.author","Nitta, A."],["dc.contributor.author","Winget, D. E."],["dc.contributor.author","Kepler, S. O."],["dc.contributor.author","Montgomery, M. H."],["dc.contributor.author","Metcalfe, T. S."],["dc.contributor.author","Oliveira, H."],["dc.contributor.author","Fraga, L."],["dc.contributor.author","da Costa, AFM"],["dc.contributor.author","Costa, JES"],["dc.contributor.author","Castanheira, B. G."],["dc.contributor.author","Giovannini, O."],["dc.contributor.author","Nather, R. E."],["dc.contributor.author","Mukadam, A. S."],["dc.contributor.author","Kawaler, Steven D."],["dc.contributor.author","O'Brien, M. S."],["dc.contributor.author","Reed, M. D."],["dc.contributor.author","Kleinman, S. J."],["dc.contributor.author","Provencal, J. L."],["dc.contributor.author","Watson, T. K."],["dc.contributor.author","Kilkenny, D."],["dc.contributor.author","Sullivan, D. J."],["dc.contributor.author","Sullivan, T."],["dc.contributor.author","Shobbrook, B."],["dc.contributor.author","Jiang, X. J."],["dc.contributor.author","Ashoka, B. N."],["dc.contributor.author","Seetha, S."],["dc.contributor.author","Leibowitz, E. M."],["dc.contributor.author","Ibbetson, P."],["dc.contributor.author","Mendelson, H."],["dc.contributor.author","Meistas, E. G."],["dc.contributor.author","Kalytis, R."],["dc.contributor.author","Alisauskas, D."],["dc.contributor.author","O'Donoghue, D."],["dc.contributor.author","Buckley, D."],["dc.contributor.author","Martinez, P."],["dc.contributor.author","van Wyk, F."],["dc.contributor.author","Stobie, R."],["dc.contributor.author","Marang, F."],["dc.contributor.author","van Zyl, L."],["dc.contributor.author","Ogloza, W."],["dc.contributor.author","Krzesinski, J."],["dc.contributor.author","Zola, S."],["dc.contributor.author","Moskalik, P."],["dc.contributor.author","Breger, M."],["dc.contributor.author","Stankov, A."],["dc.contributor.author","Silvotti, Roberto"],["dc.contributor.author","Piccioni, A."],["dc.contributor.author","Vauclair, G."],["dc.contributor.author","Dolez, N."],["dc.contributor.author","Chevreton, M."],["dc.contributor.author","Deetjen, J."],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Perez, JMG"],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","Ulla, A."],["dc.contributor.author","Manteiga, M."],["dc.contributor.author","Suarez, O."],["dc.contributor.author","Burleigh, M. R."],["dc.contributor.author","Barstow, M. A."],["dc.date.accessioned","2018-11-07T11:18:05Z"],["dc.date.available","2018-11-07T11:18:05Z"],["dc.date.issued","2005"],["dc.description.abstract","BPM 37093 is the only hydrogen-atmosphere white dwarf currently known which has sufficient mass (similar to 1.1 M-.) to theoretically crystallize while still inside the ZZ Ceti instability strip (T-eff similar to 12 000 K). As a consequence, this star represents our first opportunity to test crystallization theory directly. If the core is substantially crystallized, then the inner boundary for each pulsation mode will be located at the top of the solid core rather than at the center of the star, affecting mainly the average period spacing. This is distinct from the \"mode trapping\" caused by the stratified surface layers, which modifies the pulsation periods more selectively. In this paper we report on Whole Earth Telescope observations of BPM 37093 obtained in 1998 and 1999. Based on a simple analysis of the average period spacing we conclude that a large fraction of the total stellar mass is likely to be crystallized."],["dc.identifier.doi","10.1051/0004-6361:20041125"],["dc.identifier.fs","38252"],["dc.identifier.isi","227493100024"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9872"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/54959"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","E D P Sciences"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Whole Earth Telescope observations of BPM 37093: A seismological test of crystallization theory in white dwarfs"],["dc.title.original","9872"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]