High-resolution optical spectroscopy of the F supergiant protoplanetary nebula IRAS 18095+2704

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ŞAHİN T., Lambert D. L., Klochkova V. G., Tavolganskaya N. S.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, cilt.410, sa.1, ss.612-626, 2011 (SCI-Expanded) identifier identifier

  • Yayın Türü: Makale / Tam Makale
  • Cilt numarası: 410 Sayı: 1
  • Basım Tarihi: 2011
  • Doi Numarası: 10.1111/j.1365-2966.2010.17467.x
  • Dergi Adı: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
  • Derginin Tarandığı İndeksler: Science Citation Index Expanded (SCI-EXPANDED), Scopus
  • Sayfa Sayıları: ss.612-626
  • Anahtar Kelimeler: stars: abundances, stars: AGB and post-AGB, stars: late-type, ATOMIC TRANSITION-PROBABILITIES, EXPERIMENTAL OSCILLATOR-STRENGTHS, METAL-POOR STARS, SOLAR ABUNDANCE, CRITICAL COMPILATION, OH/IR STARS, SILICON, SUN, LIFETIMES, EVOLUTION
  • Akdeniz Üniversitesi Adresli: Hayır

Özet

An abundance analysis is presented for IRAS 18095+2704 (V887 Her), a post-asymptotic giant branch star and protoplanetary nebula. The analysis is based on high-resolution optical spectra from the McDonald Observatory and the Special Astrophysical Observatory. Standard analysis using a classical Kurucz model atmosphere and the line analysis program moog provides the atmospheric parameters: T-eff = 6500 K, log g = +0.5, microturbulent velocity xi = 4.7 km s-1 and [Fe/H] = -0.9. Extraction of these parameters is based on excitation of Fe i lines, ionization equilibrium between neutral and ions of Mg, Ca, Ti, Cr and Fe, and the wings of hydrogen Paschen lines. Elemental abundances are obtained for 22 elements and upper limits for an additional four elements. These results show that the star's atmosphere has not experienced a significant number of C- and s-process enriching thermal pulses. Abundance anomalies as judged relative to the compositions of unevolved and less-evolved normal stars of a similar metallicity include Al, Y and Zr deficiencies with respect to Fe of about 0.5 dex. Judged by composition, the star resembles an RV Tauri variable that has been mildly affected by dust-gas separation reducing the abundances of the elements of highest condensation temperature. This separation may occur in the stellar wind. There are indications that the standard one-dimensional local thermodynamic equilibrium analysis is not entirely appropriate for IRAS 18095+2704. These include a supersonic macroturbulent velocity of 23 km s-1, emission in H alpha and the failure of predicted profiles to fit observed profiles of H beta and H gamma.

An abundance analysis is presented for IRAS 18095+2704 (V887 Her), a post-asymptotic giant branch star and protoplanetary nebula. The analysis is based on high-resolution optical spectra from the McDonald Observatory and the Special Astrophysical Observatory. Standard analysis using a classical Kurucz model atmosphere and the line analysis program moog provides the atmospheric parameters: Teff= 6500 K, log g=+0.5, microturbulent velocity ξ= 4.7 km s−1 and [Fe/H]=−0.9. Extraction of these parameters is based on excitation of Fe i lines, ionization equilibrium between neutral and ions of Mg, Ca, Ti, Cr and Fe, and the wings of hydrogen Paschen lines. Elemental abundances are obtained for 22 elements and upper limits for an additional four elements. These results show that the star's atmosphere has not experienced a significant number of C- and s-process enriching thermal pulses. Abundance anomalies as judged relative to the compositions of unevolved and less-evolved normal stars of a similar metallicity include Al, Y and Zr deficiencies with respect to Fe of about 0.5 dex. Judged by composition, the star resembles an RV Tauri variable that has been mildly affected by dust–gas separation reducing the abundances of the elements of highest condensation temperature. This separation may occur in the stellar wind. There are indications that the standard one-dimensional local thermodynamic equilibrium analysis is not entirely appropriate for IRAS 18095+2704. These include a supersonic macroturbulent velocity of 23 km s−1, emission in Hα and the failure of predicted profiles to fit observed profiles of Hβ and Hγ.