2014/03/11 by David F. Gray · 1 citation
Physics and Astronomy · #Stellar, planetary, and galactic studies #Astro and Planetary Science #Astronomy and Astrophysical Research #Physics #Microturbulence #Stars #Rotation (mathematics) #Astrophysics #Dispersion (optics) #Stellar rotation #Fourier transform #Asteroseismology #Astronomy #Optics #Geometry
paper · pdf · doi:10.1088/0004-6256/147/4/81
openalex publication_date 2014/03/11 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Projected rotation rates of five early A-type slowly rotating stars are measured spectroscopically to a precision of 0.2 km s −1 . A detailed Fourier analysis is done, as well as a comparison of profiles directly. Macroturbulence is needed in addition to rotation to reproduce the profile shapes. An upper limit of ≲2 km s −1 is placed on the microturbulence dispersion. Small unexplained differences between the models and the observations are seen in the sidelobe structure of the transforms. The v sin i results are: α Dra, 26.2; θ Leo, 22.5; α CMa A, 16.7; γ Gem A, 10.7; o Peg, 6.0 km s −1 . These stars are suitable as standards for measuring rotation using less fundamental methods.