2005/10/05 by W. P. Varricatt, Watson P. Varricatt, N. M. Ashok +1
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Be star #Emission spectrum #O-type star #Photometry (optics) #Physics #Spectral energy distribution #Spectral line #Spectroscopy #Stars #Stellar, planetary, and galactic studies #Wolf–Rayet star #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2005.09693.x
published as Mon.Not.Roy.Astron.Soc. 365 (2006) 127-133 · Accepted for publication in MNRAS - 7 Pages, 5 figures
arxiv created 2005/10/05 · openalex publication_date 2005/11/25 · arxiv updated 2015/06/24 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Near-infrared spectroscopy and photometry of the Wolf-Rayet star WR 143 (HD 195177) were obtained in the JHK photometric bands. High-resolution spectra observed in the J and H bands exhibit a narrow 1.083-μm He i line and the H i Paβ and Brackett series lines in emission superposed on the broad emission-line spectrum of the Wolf-Rayet star, giving strong indications of the presence of a companion. From the narrow emission lines observed, the companion is identified to be an early-type Be star. The photometric magnitudes exhibit variations in the JHK bands, which are probably due to the variability of the companion star. The flux density distribution is too steep for a Wolf-Rayet atmosphere. This is identified to be mainly due to the increasing contribution from the early-type companion star towards shorter wavelengths.