Observations of the Pulsating White Dwarf G 185–32

B G Castanheira,G Vauclair,G Pajdosz,R E Nather,N Dolez,J S Dixson,S J Kleinman,O Giovannini,J C Clemens,M Chevreton,A Bruvold,D E Winget,J E Solheim ,M A Barstow,D J Sullivan,D O’donoghue ,K Yanagida,M A Wood,E M Leibowitz ,D Koester,J L Provençal ,S D Kawaler,P Moskalik,A Kanaan,E Meištas ,Jurek Krzesiński ,T K Watson,T Mazeh,Max Katz ,Carl J Hansen ,M H Montgomery,D Buckley,S Zoła,S O Kepler,P A Bradley

doi:10.1051/0004-6361:20031567

Observations of the Pulsating White Dwarf G 185–32

B G Castanheira, G Vauclair + Show 33 more

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https://doi.org/10.1051/0004-6361:20031567

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Journal: Astronomy & Astrophysics	Publication Date: Dec 18, 2003
Citations: 21

Affiliation: Universidade Federal do Rio Grande do Sul, Observatoire Midi-Pyrénées, Université Toulouse III - Paul Sabatier, French National Centre for Scientific Research, Pedagogical University of Kraków, The University of Texas at Austin, Universidade de Caxias do Sul, University of North Carolina at Chapel Hill, Paris Observatory, UiT The Arctic University of Norway, University of Leicester, Victoria University of Wellington, South African Radio Astronomy Observatory, Astronomical Observatory, Florida Institute of Technology, Tel Aviv University, Kiel University, University of Delaware, Iowa State University, Nicolaus Copernicus Astronomical Center, Universidade Federal de Santa Catarina, Vilnius University, Southwestern University, Joint Institute for Laboratory Astrophysics, University of Colorado Boulder, University of Cambridge, Los Alamos National Laboratory

#Space Telescope Faint Object Spectrograph #Hubble Space Telescope Faint Object + Show 8 more

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Abstract

We observed the pulsating hydrogen atmosphere white dwarf G 185-32 with the Whole Earth Telescope in 1992. We report on a weighted Fourier transform of the data detecting 18 periodicities in its light curve. Using the Hubble Space Telescope Faint Object Spectrograph time resolved spectroscopy, and the wavelength dependence of the relative amplitudes, we identify the spherical harmonic degree (� ) for 14 pulsation signals. We also compare the determinations of effective temperature and surface gravity using the excited modes and atmospheric methods, obtaining Teff = 11 960 ± 80 K, log g = 8.02 ± 0.04 and M = 0.617 ± 0.024 M� .

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