2005/11/30 by P. L. Dufton, R. S. I. Ryans, S. Simon-Diaz +3
Mathematics · Physics and Astronomy · #Angular velocity #Astronomical and nuclear sciences #Astronomy #Astrophysics #Classical mechanics #Geometry #Line (geometry) #Mathematics #Physics #Rotation (mathematics) #Small Magellanic Cloud #Spectral line #Spectral resolution #Stars #Stellar classification #Stellar, planetary, and galactic studies #Supergiant #astro-ph
paper · pdf · doi:10.1051/0004-6361:20054600
4 figures, 8 pages, submitted to Astronomy and Astrophysics
arxiv created 2006/02/14 · openalex publication_date 2006/05/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
High-resolution spectra for 24 SMC and Galactic B-type supergiants have been analysed to estimate the contributions of both macroturbulence and rotation to the broadening of their metal lines. Two different methodologies are considered, viz. goodness-of-fit comparisons between observed and theoretical line profiles and identifying zeros in the Fourier transforms of the observed profiles. The advantages and limitations of the two methods are briefly discussed with the latter techniques being adopted for estimating projected rotational velocities (v sin i) but the former being used to estimate macroturbulent velocities. The projected rotational velocity estimates range from approximately 20 to 60 km s-1, apart from one SMC supergiant, Sk 191, with a v sin i 90 km s-1. Apart from Sk 191, the distribution of projected rotational velocities as a function of spectral type are similar in both our Galactic and SMC samples with larger values being found at earlier spectral types. There is marginal evidence for the projected rotational velocities in the SMC being higher than those in the Galactic targets but any differences are only of the order of 5–10 km s-1, whilst evolutionary models predict differences in this effective temperature range of typically 20 to 70 km s-1. The combined sample is consistent with a linear variation of projected rotational velocity with effective temperature, which would imply rotational velocities for supergiants of 70 km s-1 at an effective temperature of 28 000 K (approximately B0 spectral type) decreasing to 32 km s-1 at 12 000 K (B8 spectral type). For all targets, the macroturbulent broadening would appear to be consistent with a Gaussian distribution (although other distributions cannot be discounted) with an half-width varying from approximately 20 km s-1 at B8 to 60 km s-1 at B0 spectral types.