Analysis of the spectra of Sirius and VEGA in the 3600 to 4200 angstrom region

Details Analysis of the spectra of Sirius and VEGA in the 3600 to 4200 angstrom region Analysis of the spectra of Sirius and VEGA in the 3600 to 4200 angstrom region

Feb 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982pasp...94...50b&link_type=abstract

Astronomical Society of the Pacific, Publications, vol. 94, Feb. 1982, p. 50-54.

Astronomy and Astrophysics

Astronomy

10

A Stars, Balmer Series, Near Ultraviolet Radiation, O Stars, Spectrum Analysis, Stellar Spectra, White Dwarf Stars, Atmospheric Models, Radiant Flux Density, Stellar Atmospheres, Stellar Models, Stellar Spectrophotometry, Stellar Temperature, Ubv Spectra

Scientific paper

A comparison between the spectral properties of Vega and Sirius and theoretical predictions of flux constant line-blanketed atmospheric models in the wavelength region just longward of the Balmer limit (3600 to 4200 A) is presented in light of the use of Vega as a zero point star for stellar property determination. Synthetic spectra were calculated from models of Vega with effective temperature between 9300 and 10,000 K, log g of 3.5 or 4.0 and A/H concentration ratio 0.0, and models of Sirius of effective temperature 10,000 to 10,250 K, log g 4.0 or 4.3, and A/H concentration ratio 0.5. The best models of the respective stars are found to agree with the observations to within 10% or better. It is also estimated that when Vega is used as a zero-point star for color calculations, differences between theoretical and observed color systems of 0.07 magnitudes will result in the 37-52 color index of the Johnson and Mitchell system, and 0.03 magnitude in (U-B) of the UBV system.

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