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Title:
Whole Earth Telescope observations of BPM 37093: A seismological test of crystallization theory in white dwarfs
Authors:
Kanaan, A.; Nitta, A.; Winget, D. E.; Kepler, S. O.; Montgomery, M. H.; Metcalfe, T. S.; Oliveira, H.; Fraga, L.; da Costa, A. F. M.; Costa, J. E. S.; Castanheira, B. G.; Giovannini, O.; Nather, R. E.; Mukadam, A.; Kawaler, S. D.; O'Brien, M. S.; Reed, M. D.; Kleinman, S. J.; Provencal, J. L.; Watson, T. K.; Kilkenny, D.; Sullivan, D. J.; Sullivan, T.; Shobbrook, B.; Jiang, X. J.; Ashoka, B. N.; Seetha, S.; Leibowitz, E.; Ibbetson, P.; Mendelson, H.; Meištas, E. G.; Kalytis, R.; Ališauskas, D.; O'Donoghue, D.; Buckley, D.; Martinez, P.; van Wyk, F.; Stobie, R.; Marang, F.; van Zyl, L.; Ogloza, W.; Krzesinski, J.; Zola, S.; Moskalik, P.; Breger, M.; Stankov, A.; Silvotti, R.; Piccioni, A.; Vauclair, G.; Dolez, N.; Chevreton, M.; Deetjen, J.; Dreizler, S.; Schuh, S.; Gonzalez Perez, J. M.; Østensen, R.; Ulla, A.; Manteiga, M.; Suarez, O.; Burleigh, M. R.; Barstow, M. A.
Affiliation:
AA(Departamento de Física Universidade Federal de Santa Catarina, CP 476, 88040-900 Florianópolis, SC, Brazil ), AB(Apache Point Observatory, 2001 Apache Point Road, PO Box 59, Sunspot, NM 88349, USA), AC(Department of Astronomy, 1 University Station Stop C1400, University of Texas, Austin, TX 78712, USA), AD(Instituto de Física, Universidade Federal de Rio Grande do Sul, CP 10501, 91501-970 Porto Alegre, RS, Brazil), AE(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK ; Department of Astronomy, 1 University Station Stop C1400, University of Texas, Austin, TX 78712, USA), AF(Harvard-Smithsonian Center for Astrophysics, USA ; Department of Astronomy, 1 University Station Stop C1400, University of Texas, Austin, TX 78712, USA), AG(Departamento de Física Universidade Federal de Santa Catarina, CP 476, 88040-900 Florianópolis, SC, Brazil), AH(Departamento de Física Universidade Federal de Santa Catarina, CP 476, 88040-900 Florianópolis, SC, Brazil), AI(Instituto de Física, Universidade Federal de Rio Grande do Sul, CP 10501, 91501-970 Porto Alegre, RS, Brazil), AJ(Instituto de Física, Universidade Federal de Rio Grande do Sul, CP 10501, 91501-970 Porto Alegre, RS, Brazil), AK(Instituto de Física, Universidade Federal de Rio Grande do Sul, CP 10501, 91501-970 Porto Alegre, RS, Brazil), AL(Departamento de Fisica e Quimica, UCS, Brazil), AM(Department of Astronomy, 1 University Station Stop C1400, University of Texas, Austin, TX 78712, USA), AN(Department of Astronomy, 1 University Station Stop C1400, University of Texas, Austin, TX 78712, USA), AO(Dept. of Physics & Astronomy, Iowa State University, USA), AP(Dept. of Physics & Astronomy, Iowa State University, USA), AQ(Dept. of Physics & Astronomy, Iowa State University, USA ; Astronomy Dept., Southwest Missouri State University, USA), AR(Apache Point Observatory, 2001 Apache Point Road, PO Box 59, Sunspot, NM 88349, USA), AS(Dept. of Physics & Astronomy, University of Delaware, USA), AT(Southwestern University, Georgetown, TX, USA), AU(South African Astronomical Observatory, South Africa), AV(Victoria University of Wellington, New Zealand), AW(Victoria University of Wellington, New Zealand), AX(Chatterton Astronomy Dept., University of Sydney, Australia), AY(Astronomical Observatory, Academy of Sciences, PR China), AZ(Indian Space Research Organization, India), BA(Indian Space Research Organization, India), BB(Wise Observatory, Tel-Aviv University, Israel), BC(Wise Observatory, Tel-Aviv University, Israel), BD(Wise Observatory, Tel-Aviv University, Israel), BE(Institute of Theoretical Physics & Astronomy, Lithuania), BF(Institute of Theoretical Physics & Astronomy, Lithuania), BG(Vilnius University, Lithuania), BH(South African Astronomical Observatory, South Africa), BI(South African Astronomical Observatory, South Africa), BJ(South African Astronomical Observatory, South Africa), BK(South African Astronomical Observatory, South Africa), BL(South African Astronomical Observatory, South Africa), BM(South African Astronomical Observatory, South Africa), BN(South African Astronomical Observatory, South Africa), BO(Mt. Suhora Observatory, Cracow Pedagogical University, Poland), BP(Mt. Suhora Observatory, Cracow Pedagogical University, Poland), BQ(Mt. Suhora Observatory, Cracow Pedagogical University, Poland ; Astronomical Observatory, Jagiellonia University, Poland), BR(Copernicus Astronomical Center, Poland), BS(Institut für Astronomie, Universität Wien, Austria), BT(Institut für Astronomie, Universität Wien, Austria), BU(INAF - Osservatorio Astronomico di Capodimonte, Italy), BV(Dipartimento di Astronomia, Università di Bologna, Italy), BW(Université Paul Sabatier, Observatoire Midi-Pyrénées, France), BX(Université Paul Sabatier, Observatoire Midi-Pyrénées, France), BY(Observatoire de Paris-Meudon, France), BZ(Institut für Astronomie und Astrophysik, Germany), CA(Institut für Astronomie und Astrophysik, Germany ; Universitätssternwarte Göttingen, Germany), CB(Institut für Astronomie und Astrophysik, Germany ; Universitätssternwarte Göttingen, Germany), CC(University of Tromsø, Norway), CD(Isaac Newton Group, Spain), CE(Departamento de Física Aplicada, Universidad de Vigo, Spain), CF(Departamento de Física Aplicada, Universidad de Vigo, Spain), CG(Departamento de Física Aplicada, Universidad de Vigo, Spain), CH(Dept. of Physics & Astronomy, University of Leicester, UK), CI(Dept. of Physics & Astronomy, University of Leicester, UK)
Publication:
Astronomy and Astrophysics, Volume 432, Issue 1, March II 2005, pp.219-224 (A&A Homepage)
Publication Date:
03/2005
Origin:
A&A
Keywords:
stars: evolution, stars: individual: BPM 37093, stars: interiors, stars: oscillations, white dwarfs
DOI:
10.1051/0004-6361:20041125
Bibliographic Code:
2005A&A...432..219K

Abstract

BPM 37093 is the only hydrogen-atmosphere white dwarf currently known which has sufficient mass (~1.1 Mȯ) to theoretically crystallize while still inside the ZZ Ceti instability strip (Teff˜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.

Based on observations obtained at: Observatório do Pico dos Dias (OPD) Brazil, the European Southern Observatory (ESO) Chile, South African Astronomical Observatory (SAAO), Mt. John University Observatory (MJUO) New Zealand, Siding Spring Observatory (SSO) Australia, and Cerro Tololo Inter-American Observatory (CTIO), a division of the National Optical Astronomy Observatories, which is operated by the Association of Universities for Research in Astronomy, Inc. under cooperative agreement with the National Science Foundation.


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