A High-resolution Study of the Spectrum of HD 190073 (V1295 Aql)

Details A High-resolution Study of the Spectrum of HD 190073 (V1295 Aql) A High-resolution Study of the Spectrum of HD 190073 (V1295 Aql)

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21711305c&link_type=abstract

American Astronomical Society, AAS Meeting #217, #113.05; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

Detailed abundance work on Herbig Ae stars began in the last decade. Acke and Waelkens's (A&A, 427, 1009, 2004, henceforth AW) study is exemplary. We report results for HD 190073 (V1295 Aql), based on significantly better spectroscopic material: 8 averaged HARPS spectra from the ESO archive (RP=110,000, Fourier-filtered, S/N 200-350).
There is significant line emission, not only in the Balmer cores, but also in myriad metal lines. We assume with AW that abundances may be derived from equivalent widths of lines not involved with emission, taken to belong to a photosphere not badly deviant from models. We confirm AW for HD 190073, in that consistent results may be obtained from two stages of ionization of several elements, and internal excitations within an ionization
stage. We adopt Teff=9100K, and log(g)=3.0, slightly different from AW's 9250K and log(g)=3.5. The adopted parameters give fits to the wings of the Balmer lines. We find no indication of anomalous saturation found for HD 101412 (A&A, in press, arXiv:1008.1601), in spite of the far more prominent emission of HD 190073. The latter star is more massive, and younger, and probably observed nearly pole on.
The iron abundance is closely solar, but we find a larger nitrogen excess than AW, +0.8 dex. Sodium is in excess by the same amount, while zinc is overabundant by 0.3 dex.
The emission-line spectrum was described recently by Catala, et al. (A&A, 462, 293, 1967). We model the region as a hot slab above an approximate stellar photosphere. Metallic emission below the Balmer jump is often optically thick, while the line centers rarely approach unit optical depth above it.

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