The absolute energy distributions of the sun, of the 'solar analogs' 16 CYG B, Hyades VB 64, 16 CYG A, and of the standard stars Alpha LYR and 29 PSC

Details The absolute energy distributions of the sun, of the 'solar analogs' 16 CYG B, Hyades VB 64, 16 CYG A, and of the standard stars Alpha LYR and 29 PSC The absolute energy distributions of the sun, of the 'solar analogs' 16 CYG B, Hyades VB 64, 16 CYG A, and of the standard stars Alpha LYR and 29 PSC

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...159..175n&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 159, no. 1-2, April 1986, p. 175-188.

Astronomy and Astrophysics

Astrophysics

26

Solar Spectra, Spectral Energy Distribution, Stellar Spectra, Analogs, Solar Flux, Stellar Magnitude, Ubv Spectra

Scientific paper

The absolute energy distributions of the solar analog 16 Cyg B, which have been published by Hardorp (1980b) and Taylor (1984a), are compared with the Sun's absolute energy distribution by Neckel and Labs (1984). To avoid any passband mismatches, the absolutely calibrated (Neckel and Labs, 1984) version of the high resolution solar flux atlas of Kurucz et al. (1984) was used to derive solar magnitudes for exactly the same passbands that were used for the stellar measurements. The magnitude differences star minus Sun reveal an overall, λ/1-proportional gradient corresponding to Δ(Θ) = Δ(5040/T) ≍ 0.009 ± 0.002, on which is superimposed a wavy pattern with amplitudes being generally near 0.m02. At a few wavelengths one or the other stellar data set - but never both - yields residuals up to 0.m04. Regarding also the differences (a) between observed and model-predicted energy distributions, (b) between 'old' and 'new' energy distribution of α Lyr, and (c) between the energy distributions of different solar analogs, it seems that most if not all of the wavy pattern is caused by systematic, wavelength-dependent errors originating somewhere in the long sequence of observations rather than by genuine characteristics of the stellar or solar radiation. Supposing then that the 'true' 16 Cyg B minus Sun differences run as smoothly as the observed differences between 16 Cyg B and other solar-type stars (e.g. 16 Cyg A), and allowing for remaining errors in the absolute energy distributions involved, the solar UBV-colors should lie within the following limits (see Table 4): (B - V)sun = 0.m650 ± O.m005, (U - B)sun = O.m195 ± O.m005. With VαLyr = 0.m03 and V16CygB = 6.m20 we get Vsun = - 26.m75; its error is presumably less than ± 0.m025.

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