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ABUNDANCES OF MERCURY IN SIRIUS AND VEGA

ABUNDANCES OF MERCURY IN SIRIUS AND VEGA The resonance line of Hg II at 1942 Å in Sirius and Vega is analyzed quantitatively based on high-resolution UV spectroscopic data. The spectrum synthesis technique is employed. The abundance of Hg in Sirius (log ∊(Hg) = 2.5±0.5) is found to coincide with that found in the two normal late B-type stars ν Cap and π Cet. On the other hand, the obtained upper limit for Vega (log ∊(Hg) ≤ 0.5) is lower than the solar-system abundance log ∊(Hg) = 1.2. http://www.deepdyve.com/assets/images/DeepDyve-Logo-lg.png Publications of the Astronomical Society of the Pacific IOP Publishing

ABUNDANCES OF MERCURY IN SIRIUS AND VEGA

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Copyright
Copyright © 1988. The Astronomical Society of the Pacific. All rights reserved. Printed in U.S.A.
ISSN
0004-6280
eISSN
1538-3873
DOI
10.1086/132239
Publisher site
See Article on Publisher Site

Abstract

The resonance line of Hg II at 1942 Å in Sirius and Vega is analyzed quantitatively based on high-resolution UV spectroscopic data. The spectrum synthesis technique is employed. The abundance of Hg in Sirius (log ∊(Hg) = 2.5±0.5) is found to coincide with that found in the two normal late B-type stars ν Cap and π Cet. On the other hand, the obtained upper limit for Vega (log ∊(Hg) ≤ 0.5) is lower than the solar-system abundance log ∊(Hg) = 1.2.

Journal

Publications of the Astronomical Society of the Pacific – IOP Publishing

Published: Jul 1, 1988

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