Elemental abundance analyses with DAO spectrograms: XXXII. HR 6455 (A3 III), δ Aqr (A3 V), η Lep (F2 V), and 1 Boo (A1 V)

• Published in: Astronomische Nachrichten Vol. 332; no. 7; pp. 681 - 689
• Main Authors: Yüce, K., Adelman, S.J., Gulliver, A.F., Hill, G.
• Format: Journal Article
• Language: English
• Published: Berlin WILEY-VCH Verlag 01.08.2011; WILEY‐VCH Verlag
• Subjects: 1 Boo; stars: abundances; stars: individual (HR 6455; stars: individual (HR 6455, δ Aqr, η Lep, 1 Boo); δ Aqr; η Lep
• ISSN: 0004-6337; 1521-3994
• DOI: 10.1002/asna.201111575

We examine the sharp‐lined stars HR 6455 (A3 III, v sin i = 8.7 km s–1) and η Lep (F2 V, v sin i = 13.5 km s–1) as well as δ Aqr (A3 V, v sin i = 81 km s–1) and 1 Boo (A1 V, v sin i = 59 km s–1) to increase the number consistently analyzed A and F stars using high dispersion and high S/N (≥200) spectrograms obtained with CCD detectors at the long Coudé camera of the 1.22‐m telescope of the Dominion Astrophysical Observatory. Such studies contribute to understanding systematic abundance differences between normal and non‐magnetic main‐sequence band chemically peculiar A and early F stars. LTE fine analyses of HR 6455, δ Aqr, and 1 Boo using Kurucz's ATLAS suite programs show the same general elemental abundance trends with differences in the metal richness. Light and iron‐peak element abundances are generally solar or overabundant while heavy element and rare earth element abundances are overabundant. HR 6455 is an evolved Am star while δ Aqr and 1 Boo show the phenomenon to different extents. Most derived abundances of η Lep are solar (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)