Chemical composition of the CP Hg-Mn components of approximately equal mass in the SB2 system 46 Draconis

Details Chemical composition of the CP Hg-Mn components of approximately equal mass in the SB2 system 46 Draconis Chemical composition of the CP Hg-Mn components of approximately equal mass in the SB2 system 46 Draconis

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998astl...24...90t&link_type=abstract

Astronomy Letters, Volume 24, Issue 1, January 1998, pp.90-105; Pis'ma v Astronomicheskii Zhurnal, Vol. 24, p. 116

Astronomy and Astrophysics

Astronomy

2

Scientific paper

We have performed the most complete (to date) atmospheric-abundance analysis of the components of approximately equal mass in the SB2 system 46 Dra using the high-resolution, S/N = > 200 CCD spectra obtained with the echelle spectrograph of the 2.7-m McDonald Observatory telescope. The abundances of 25 elements were determined from lines in the wide spectral range 3800 to 9000 A. The rotation of the components is shown to be synchronized and coaxial with the orbital motion. The chemical anomalies of both components were found to be generally similar: an underabundance of He, C, N, O, and Al; a nearly solar abundance of iron-peak elements; and considerable overabundances of P, Mn, Ga, Sr, Y, Zr, Ba, Pt, Au, and Hg, which increase with increasing atomic number. However, we found significant differences in the abundances of some elements in components A and B, similar to those that were previously detected in the analogous SB2 system ARAur: an underabundance of Al and Ni in component A with a smaller anomaly or a normal abundance of these two elements in component B. Component A shows a considerably greater overabundance of Ga and considerably smaller overabundances of Sr and Pt than component B does.There are also differences between the systems themselves: in contrast to AR Aur, in which only component A exhibits great overabundances of Y, Ba, and Hg, these elements are equally greatly enhanced in both components of 46 Dra. The most striking difference between components A and B of 46 Dra, which are similar in all physical parameters, is the difference in the isotopic composition of mercury which was first detected by Cowley and Aikman (1975) and confirmed in this study. It is concluded that the abundance difference between the components could arise after the synchronization of the rotation and the arrival of the stars at the main sequence.

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