Quantitative Analysis and Spectral Variation of the Ap Star HD 151 199

Details Quantitative Analysis and Spectral Variation of the Ap Star HD 151 199 Quantitative Analysis and Spectral Variation of the Ap Star HD 151 199

Jan 1970

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1970ap%26ss...6..141g&link_type=abstract

Astrophysics and Space Science, Volume 6, Issue 1, pp.141-153

Astronomy and Astrophysics

Astrophysics

2

Scientific paper

The radial velocity, intensity variations of the Ca ii line and chemical composition of the suspected magnetic star HD 151 199 have been studied using three 9.6 A/mm and twenty-one 40 A/mm dispersion spectrograms which were taken at St. Michel and Asiago Observatories respectively. The radial velocity and the intensity of the Ca ii K line suggest a variation with a 6.143 day period. The range is about 40 km/sec for the radial velocity and the K line changes in intensity by 50%. Preliminary results of the photometric data in the Geneva system show a similar trend of variation in Δ (B 2-B 1) with the same period. Hβ and Hγ contours and the Balmer discontinuity give θeff=0.50 and logg=4. The most probable microturbulence is found to be 6.4 km/sec. The excitation temperature, θexc=0.50, is derived from the Fe lines and adopted for the other elements as well. A quantitative analysis by curve of growth and weighting function method, using Mihalas and Conti's atmospherical models was made. HD 151 199 shows an overabundance of Ca, Sr, Ba, by factors of 2, 40, and 5 with respect to 30 L Mi. Eu ii is probably overabundant also but it is not possible to give this element a numerical value. The other elements seem to be normal.

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