Iron and magnesium in the white dwarf GD 40 - A test of diffusion theory

Details Iron and magnesium in the white dwarf GD 40 - A test of diffusion theory Iron and magnesium in the white dwarf GD 40 - A test of diffusion theory

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...266..761s&link_type=abstract

Astrophysical Journal, Part 1, vol. 266, Mar. 15, 1983, p. 761-768. No. AST-81-15095;

Astronomy and Astrophysics

Astrophysics

33

Abundance, Diffusion Theory, Metallicity, Stellar Mass Accretion, Ultraviolet Spectra, White Dwarf Stars, Iron, Iue, Line Spectra, Magnesium, Stellar Atmospheres, Stellar Spectra, Stellar Temperature

Scientific paper

An outstanding problem in interpreting the properties of white-dwarf stars is related to the understanding of the chemical abundances in their atmospheres. The hydrogen-rich white-dwarf stars have monoelemental atmospheres, with small quantities of helium and no heavier elements observed in most, possibly all, stars with visible H lines. The helium-rich stars are more complex, and the existence of metallic lines in many of their spectra is now well confirmed. The DB star GD 40 (Gr 384) is the hottest He-rich white-dwarf star to show metal lines, apart from the extremely hot objects, such as HZ 21 and HD 149499B. The present investigation is concerned with IUE spectra which have been obtained of the GD 40. It is found that the near-UV is marked by strong Mg II lines along with broad blends of Fe II lines. An analysis is conducted of the abundances of Fe and Mg at the surface of GD 40 using a limited spectrum-synthesis technique with the measured equivalent widths of the best Fe II features.

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