Determining rotational and macroturbulent velocities of cool magnetic giant stars

Abstract

An original method of estimating the projected rotational velocity, $vsini$, and the macroturbulent velocity, $v_{\mathrm{mac}}$, of evolved M giant stars is presented. It is based on the use of spectrum synthesis and multi-line analysis tools. The goal is to fit the mean line profile of observations with that of synthetic spectra. The method is applied to the red giant star RZ Ari and the results $v\sin i$ = 6.0 $\pm$ 0.5 km/s and $v_{\mathrm{mac}}$ = 2.0 $\pm$ 1.0 km/s are obtained.

References in corpus (6)

• A grid of MARCS model atmospheres for late-type stars I. Methods and general properties
• The surprising magnetic topology of tauSco: fossil remnant or dynamo output?
• The atmospheric parameters and spectral interpolator for the stars of MILES
• Rotational velocities of the giants in symbiotic stars: II. Are S-type symbiotics synchronized?
• Direct detection of a magnetic field in the photosphere of the single M giant EK Boo: How common is magnetic activity among M giants?
• Rotational velocities of the giants in symbiotic stars: III. Evidence of fast rotation in S-type symbiotics

Cited by in corpus (1)

• Surface magnetism in the pulsating RV Tauri star R Scuti