A line profile analysis of the pulsating red giant star Ophiuchi (G9.5III)
Sheffield, UK : ESA Publications Division
InThompson, M.; Fletcher, K. (ed.), SOHO 18/GONG 2006/HELAS I, Beyond the spherical Sun (ESA SP-624), pp. 117
Article in monograph or in proceedings
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Thompson, M.; Fletcher, K. (ed.), SOHO 18/GONG 2006/HELAS I, Beyond the spherical Sun (ESA SP-624)
So far, solar-like oscillations have been studied using radial velocity and/or light curve variations, which reveal frequencies of the oscillation modes. Line-profile variations, however, are also a valuable diagnostic to characterise radial and non-radial oscillations, including frequencies, amplitudes, the spherical mode wavenumbers (l,m) and the stellar inclination angle. Here we present a line profile analysis of epsilon Ophiuchi, which is a pulsating red giant. The main differences compared to previous line profile analyses done for heat-driven oscillations are the small amplitudes and the predicted short damping and re-excitation times in red giants. Two line diagnostics have been tested to see whether these are sensitive to the small line profile variations present in red giants. In addition, line profiles have been simulated with short damping and re-excitation times and are compared with the observations. This comparison reveals that non-radial modes are detected in the observed line profile variations of epsilon Ophiuchi. This is rather surprising, as theoretical predictions favours the occurrence of radial modes.
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