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Title:
Understanding the Cool DA White Dwarf Pulsator, G29-38
Authors:
Kleinman, S. J.; Nather, R. E.; Winget, D. E.; Clemens, J. C.; Bradley, P. A.; Kanaan, A.; Provencal, J. L.; Claver, C. F.; Watson, T. K.; Yanagida, K.; Nitta, A.; Dixson, J. S.; Wood, M. A.; Grauer, A. D.; Hine, B. P.; Fontaine, G.; Liebert, James; Sullivan, D. J.; Wickramasinghe, D. T.; Achilleos, N.; Marar, T. M. K.; Seetha, S.; Ashoka, B. N.; Meištas, E.; Leibowitz, E. M.; Moskalik, P.; Krzesiński, J.; Solheim, J.-E.; Bruvold, A.; O'Donoghue, D.; Kurtz, D. W.; Warner, B.; Martinez, Peter; Vauclair, G.; Dolez, N.; Chevreton, M.; Barstow, M. A.; Kepler, S. O.; Giovannini, O.; Augusteijn, T.; Hansen, C. J.; Kawaler, S. D.
Affiliation:
AA(New Jersey Institute of Technology, Big Bear Solar Observatory, 40386 North Shore Lane, Big Bear City, CA 92314; .; Astronomy Department, University of Texas, Austin, TX 78712.; Guest Observer, Mount Stromlo and Siding Spring Observatory, New South Wales, Australia.), AB(Astronomy Department, University of Texas, Austin, TX 78712.), AC(Astronomy Department, University of Texas, Austin, TX 78712.; Visiting Astronomer, Canada-France-Hawaii Telescope, operated by the National Research Council of Canada, Centre National de la Recherche Scientifique de France, and the University of Hawaii.), AD(Visiting Astronomer, Canada-France-Hawaii Telescope, operated by the National Research Council of Canada, Centre National de la Recherche Scientifique de France, and the University of Hawaii.; California Institute of Technology, Pasadena, CA 91125.; Fairchild Fellow.), AE(X-2, MS B-220, Los Alamos National Laboratory, Los Alamos, NM 87545.), AF(Instituto de Física, Universidade Federal do Rio Grande do Sul, 91501-970 Porto Alegre-RS, Brazil.; Guest Observer, Isaac Newton Telescope, Roque de los Muchachos, La Palma, Canaries.), AG(University of Delaware, Physics and Astronomy Department, Sharp Laboratory, Newark, DE 19716.; Guest Observer, Cerro Tololo Inter-American Observatory, Chile.), AH(NOAO, 950 North Cherry Avenue, Tucson, AZ 85726.), AI(Department of Physics and Astronomy, Iowa State University, Ames, IA 50211.), AJ(Astronomy Department, University of Texas, Austin, TX 78712.; Current postal address: 5-35-11 Hongōdai, Sakae-ku Yokohama 247, Japan.), AK(Astronomy Department, University of Texas, Austin, TX 78712.), AL(M/S ADVP3, DSC Communications Corporation, 1000 Coit Road, Plano, TX 75075.), AM(Department of Physics and Space Sciences, Florida Institute of Technology, 150 West University Boulevard, Melbourne, FL 32901.; Guest Observer, Institute for Astronomy, Honolulu, HI.), AN(Department of Physics and Astronomy, University of Arkansas, Little Rock, AR 72204.; Visiting Astronomer, Kitt Peak National Observatory.), AO(NASA Ames Research Center, MS 269-3, Moffett Field, CA 94035.), AP(Visiting Astronomer, Canada-France-Hawaii Telescope, operated by the National Research Council of Canada, Centre National de la Recherche Scientifique de France, and the University of Hawaii.; Department de Physique, Université de Montréal, C.P. 6128, Montreal, PQ, H3C 3J7 Canada.), AQ(Steward Observatory, University of Arizona, Tucson, AZ 85721.), AR(Department of Physics, Victoria University, Box 600, Wellington, New Zealand.), AS(Department of Mathematics, Australia National University, Canberra, Australia.), AT(Department of Mathematics, Australia National University, Canberra, Australia.), AU(Indian Space Research Organization, Bangalore 560 017, India.), AV(Indian Space Research Organization, Bangalore 560 017, India.), AW(Indian Space Research Organization, Bangalore 560 017, India.), AX(Institute of Theoretical Physics and Astronomy, Goštauto 12, Vilnius 2600, Lithuania.; Guest Observer, Maidanak Observatory, Uzbekistan.), AY(Department of Physics and Astronomy, University of Tel Aviv, Ramat Aviv, Tel Aviv 69978, Israel.), AZ(Copernicus Astronomical Center, Warsaw, Poland.), BA(Mount Suhora Observatory, Cracow Pedagogical University, ul. Podchorżych 2, 30-084 Cracow, Poland.), BB(Guest Observer, Maidanak Observatory, Uzbekistan.; Institutt for Matematiske Realfag, Universitet i Tromso, 9000 Tromso, Norway.), BC(Institutt for Matematiske Realfag, Universitet i Tromso, 9000 Tromso, Norway.), BD(Department of Astronomy, University of Cape Town, Rondebosch 7700, Cape Province, South Africa.), BE(Department of Astronomy, University of Cape Town, Rondebosch 7700, Cape Province, South Africa.), BF(Department of Astronomy, University of Cape Town, Rondebosch 7700, Cape Province, South Africa.), BG(Department of Astronomy, University of Cape Town, Rondebosch 7700, Cape Province, South Africa.), BH(Observatoire Midi-Pyrenees, 14 Avenue E. Belin, 31400 Toulouse, France.), BI(Observatoire Midi-Pyrenees, 14 Avenue E. Belin, 31400 Toulouse, France.), BJ(Observatoire de Paris-Meudon, F-92195 Meudon, Principal Cedex, France.), BK(Guest Observer, Isaac Newton Telescope, Roque de los Muchachos, La Palma, Canaries.; Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK.; PPARC Advanced Fellow.), BL(Instituto de Física, Universidade Federal do Rio Grande do Sul, 91501-970 Porto Alegre-RS, Brazil.), BM(Instituto de Física, Universidade Federal do Rio Grande do Sul, 91501-970 Porto Alegre-RS, Brazil.; Visiting Astronomer, Laboratorio Nacional de Astrofisica, CNPq, Brazil.), BN(European Southern Observatory, Casilla 19001, Santiago 19, Chile.), BO(JILA, University of Colorado, Box 440, Boulder, CO 80309.), BP(Department of Physics and Astronomy, Iowa State University, Ames, IA 50211.)
Publication:
The Astrophysical Journal, Volume 495, Issue 1, pp. 424-434. (ApJ Homepage)
Publication Date:
03/1998
Origin:
APJ; UCP
Astronomy Keywords:
STARS: INDIVIDUAL ALPHANUMERIC: G29-38, STARS: OSCILLATIONS, STARS: WHITE DWARFS, Stars: Individual: Alphanumeric: G29-38, Stars: Oscillations, Stars: White Dwarfs
Abstract Copyright:
(c) 1998: The American Astronomical Society
DOI:
10.1086/305259
Bibliographic Code:
1998ApJ...495..424K

Abstract

The white dwarfs are promising laboratories for the study of cosmochronology and stellar evolution. Through observations of the pulsating white dwarfs, we can measure their internal structures and compositions, critical to understanding post-main-sequence evolution, along with their cooling rates, which will allow us to calibrate their ages directly. The most important set of white dwarf variables to measure are the oldest of the pulsators, the cool DA variables (DAVs), which have not been explored previously through asteroseismology due to their complexity and instability. Through a time-series photometry data set spanning 10 yr, we explore the pulsation spectrum of the cool DAV, G29-38 and find an underlying structure of 19 (not including multiplet components) normal-mode, probably l=1 pulsations amidst an abundance of time variability and linear combination modes. Modeling results are incomplete, but we suggest possible starting directions and discuss probable values for the stellar mass and hydrogen layer size. For the first time, we have made sense out of the complicated power spectra of a large-amplitude DA pulsator. We have shown that its seemingly erratic set of observed frequencies can be understood in terms of a recurring set of normal-mode pulsations and their linear combinations. With this result, we have opened the interior secrets of the DAVs to future asteroseismological modeling, thereby joining the rest of the known white dwarf pulsators.
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