2006/10/26 by R. T. Zavala, Saul J. Adelman, S. J. Adelman +8 · 3 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Binary number #Binary star #Manganese #Materials science #Mercury (programming language) #Metallurgy #Observatory #Physics #Primary (astronomy) #Spectral line #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/510108
published as Astrophys.J.655:1046-1057,2007 · Accepted to ApJ, 45 pages, 11 figures
arxiv created 2006/10/26 · openalex publication_date 2007/01/23 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Observations of the mercury-manganese star ϕ Her with the Navy Prototype Optical Interferometer (NPOI) conclusively reveal the previously unseen companion in this single-lined binary system. The NPOI data were used to predict a spectral type of A8 V for the secondary star ϕ Her B. This prediction was subsequently confirmed by spectroscopic observations obtained at the Dominion Astrophysical Observatory. ϕ Her B is rotating at 50 ± 3 km s -1 , in contrast to the 8 km s -1 lines of ϕ Her A. Recognizing the lines from the secondary permits one to separate them from those of the primary. The abundance analysis of ϕ Her A shows an abundance pattern similar to those of other HgMn stars, with Al being very underabundant and Sc, Cr, Mn, Zn, Ga, Sr, Y, Zr, Ba, Ce, and Hg being very overabundant.