2012/03/20 by E. Brunsden, K. R. Pollard, P. L. Cottrell +3
Engineering · Physics and Astronomy · #Astronomical Observations and Instrumentation #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Frequency analysis #Image (mathematics) #Line (geometry) #Noise (video) #Physics #Star (game theory) #Stars #Stellar rotation #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1111/j.1365-2966.2012.20861.x
Accepted to MNRAS 2012 March 2
arxiv created 2012/03/20 · openalex publication_date 2012/04/05 · arxiv updated 2015/06/04 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present the mode identification of frequencies found in spectroscopic observations of the γ Doradus star HD 135825. Four frequencies were successfully identified: 1.3150 ± 0.0003, 0.2902 ± 0.0004, 1.4045 ± 0.0005 and 1.8829 ± 0.0005 d−1. These correspond to (l, m) modes of (1, 1), (2, −2), (4, 0) and (1, 1), respectively. Additional frequencies were found but they were below the signal-to-noise ratio limit of the Fourier spectrum and not suitable for mode identification. The rotational axis inclination and v sin i of the star were determined to be 87° (nearly edge-on) and 39.7 km s−1 (moderate for γ Doradus stars), respectively. A simultaneous fit of these four modes to the line profile variations in the data gives a reduced χ2 of 12.7. We confirm, based on the frequencies found, that HD 135825 is a bona fide γ Doradus star.