Fourier analysis of Fe I lines in the spectra of the Sun, α Centauri A, Procyon, Arcturus, and Canopus

Details Fourier analysis of Fe I lines in the spectra of the Sun, α Centauri A, Procyon, Arcturus, and Canopus Fourier analysis of Fe I lines in the spectra of the Sun, α Centauri A, Procyon, Arcturus, and Canopus

2010-04-20

arxiv.org/abs/1004.3286v1

Kinematics Phys. Celest. Bodies, 1998, Vol. 14, No. 3, p. 169-179, Kinematika Fiz. Nebesn. Tel, 1998, Tom 14, No. 3, p. 219-23

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

15 pages, 3 figures, 4 tables, published by Kinematics Phys. Celest. Bodies (in English) and Kinematika Fiz. Nebesn. Tel (in R

Scientific paper

We used spectral observations of Fe I line profiles with a 200 000 resolution to determine micro and macroturbulent velocities in the atmospheres of the Sun as a star, {\alpha} Cen A, Procyon ({\alpha} CMi), Arcturus ({\alpha} Boo), and Canopus ({\alpha} Car). Isotropic microturturbulent velocities (V_mi) and radial-tangential macroturbulent velocities (V_ma,RT) were found to be a quite suitable approximation to the velocity field in the atmospheres of all stars studied except Canopus. The average velocities V_mi and V_ma,RT are 0.8 +/- 0.1 and 2.6 +/- 0.3 km/s for the Sun as a star, 0.8 +/- 0.2 and 2.9 +/- 0.4 km/s for {\alpha} Cen A, 0.8 +/- 0.3 and 5.9 +/- 0.2 km/s for Procyon, 1.0 +/- 0.2 and 4.6 +/- 0.3 km/s for Arcturus. The velocity field in the atmosphere of Canopus can be described by an anisotropic radial-tangential distribution of microturbulence with V_mi,RT = 2.1 km/s and anisotropic distribution of macroturbulence with V_ma,rad = 17 +/- 2 km/s and V_ma,tan = 1.3 +/- 1.0 km/s. From Fourier analysis of broadening and shapes of three spectral lines of Fe I, we have derived the rotation velocity V_e sini = 3.5 +/- 0.2 km/s for Canopus.

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