Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· On-line Data
· References in the article
· Citations to the Article (13) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (4)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Mode Identification of BPM 37093 with the HST
Authors:
Nitta, A.; Kanaan, A.; Kepler, S. O.; Koester, D.; Montgomery, M. H.; Winget, D. E.
Affiliation:
AA(Astronomy Department, University of Texas, TX 78712, Austin, USA), AB(Instituto de Física, Universidade Federal de Santa Catarina, CP 476, CEP 88040-900, Florianopolis, Brazil), AC(Instituto de Física, Universidade Federal do Rio Grande do Sul, Campus do Vale, CP 15051 Goncalves, Porto Alegre, Brazil), AD(Institut für Theoretische Physik und Astrophysik, Universität Kiel, D-24098 Kiel, Germany), AE(Institut für Astronomie, Universität Wien, Türkenschanzstrasse 17, A-1180 Wien, Austria), AF(Astronomy Department, University of Texas, TX 78712, Austin, USA)
Publication:
Baltic Astronomy, v.9, p.97-112.
Publication Date:
00/2000
Origin:
BALTA
Astronomy Keywords:
STARS: INTERIORS, WHITE DWARFS, OSCILLATIONS, INDIVIDUAL: BPM 37093, ZZ CETI
Bibliographic Code:
2000BaltA...9...97N

Abstract

Theoretical calculations indicate that the massive pulsating white dwarf BPM 37093 has a crystallized interior (Winget et al. 1997, Kanaan 1996, Montgomery 1998). Crystallization was predicted theoretically about 40 years ago (Abrisokov 1961, Kirshnitz 1960; Salpeter 1961), but in spite of its importance in astrophysics, there is no direct observational evidence of the theory. Uncertainties in the nature and extent of crystallization, as well as its associated effects, are the largest sources of uncertainties in calculating the ages of the coolest white dwarf stars -- important chronometers for the Galactic disk. The Whole Earth Telescope and the Hubble Space Telescope simultaneously observed BPM 37093 in April 1999 in hopes of using asteroseismology to measure its crystallized mass fraction. The first step is correct mode identification, principally the spherical harmonic index l. Kanaan et al. (1999) explain the attempt to identify the modes from only the optical WET data, using mainly the periods of the modes. Here we present our preliminary results of applying the Robinson et al. (1995) l identification method which uses a comparison of amplitudes of the modes in the UV and in the optical spectrum.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences


More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints