Complete spectral energy distribution of the hot, helium-rich white dwarf RX J0503.9-2854
Abstract
Context. In the line-of-sight toward the DO-type white dwarf
Aims: In previous spectral analyses, many metal lines in the ultraviolet spectrum of
Methods: We compared synthetic spectra that had been calculated from model atmospheres in non-local thermodynamical equilibrium, with observations.
Results: In total, we identified 1272 lines (279 of them were newly assigned) in the wavelength range from the extreme ultraviolet to the near infrared. 287 lines remain unidentified. A close inspection of the EUV shows that still no good fit to the observed shape of the stellar continuum flux can be achieved although He, C, N, O, Al, Si, P, S, Ca, Sc, Ti, V, Cr, Mn, Fe, Cr, Ni Zn, Ga, Ge, As, Kr, Zr, Mo, Sn, Xe, and Ba are included in the stellar atmosphere models.
Conclusions: There are two possible reasons for the deviation between observed and synthetic flux in the EUV. Opacities from hitherto unconsidered elements in the model-atmosphere calculation may be missing, and/or the effective temperature is slightly lower than previously determined.
- Publication:
-
Astronomy and Astrophysics
- Pub Date:
- February 2017
- DOI:
- 10.1051/0004-6361/201629869
- arXiv:
- arXiv:1610.09177
- Bibcode:
- 2017A&A...598A.135H
- Keywords:
-
- atomic data;
- line: identification;
- stars: abundances;
- stars: individual: RX J0503.9-2854;
- virtual observatory tools;
- Astrophysics - Solar and Stellar Astrophysics
- E-Print:
- 92 pages, 45 figures