Abstract
Spectroscopic observations of stellar oscillations provide an indispensable input for asteroseismology. High-resolution and high signal-to-noise ratio time-series spectroscopy can reveal radial velocity variations as well as profile variations in stellar absorption lines which are caused by non-radial pulsations. Oscillations in solar-like stars have been detected in radial velocity measurements obtained with stabilized spectrographs. For hotter stars on the main sequence, besides for the purpose of abundance analyses, spectroscopy is mainly acquired to carry out mode identification, the assignment of the spherical degree l, and the azimuthal order m, to the observed pulsation frequencies. It has been demonstrated for several stars on the main sequence hotter than the sun that only combined spectroscopic and photometric time-series measurements can lead to successful seismic modeling. In this article, I will focus on the application of spectroscopic mode identification on pulsating stars and discuss some recent results.
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