THE BORON ABUNDANCE OF PROCYON

被引：28

作者：

LEMKE, M ^{[1
]}

LAMBERT, DL ^{[1
]}

EDVARDSSON, B ^{[1
]}

机构：

[1] ASTRON OBSERV,S-75120 UPPSALA,SWEDEN

来源：

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC | 1993年 / 105卷 / 687期

关键词：

D O I：

10.1086/133180

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The B I 2496.8 angstrom resonance line and HST/GHRS echelle spectra are used with model atmospheres and synthetic spectra to derive the B abundance of the F dwarfs Procyon (alpha Canis Minoris), theta Ursae Majoris, and iota Pegasi. The B abundance [log epsilon (B) congruent-to 2.3] of theta UMa and iota Peg is similar to that derived by Boesgaard and Heacox from the B II resonance line in spectra of A- and B-type stars. These two dwarfs show normal abundances of Li, Be, and B. Procyon, which is highly depleted in Li and Be, is depleted in B by a factor of at least 3. Comparison of the spectra of Procyon and the halo dwarf HD 140283 shows that the B abundance assigned by Duncan et al. (1992, ApJ, 401, 584) to three halo dwarfs is not greatly overestimated as a result of contamination of the B I line by an unidentified line.

引用

页码：468 / 475

页数：8

共 37 条

[1] SOLAR-SYSTEM ABUNDANCES OF THE ELEMENTS [J].