Radial Velocity Observations of Classical Pulsating Stars

TL;DR

This paper reviews the history, techniques, and recent advances in radial velocity observations of classical pulsating stars, highlighting challenges and future prospects for high-precision stellar pulsation studies.

Contribution

It provides a comprehensive overview of RV measurement techniques, recent developments, and the implications of spectral line variability for pulsating star research.

Findings

Spectral line asymmetry helps identify modulated spectral variability.

Recent developments include modulated RV curves affecting distance measurements.

Gaia's upcoming data will enhance high-precision stellar pulsation studies.

Abstract

I concisely review the history, applications, and recent developments pertaining to radial velocity (RV) observations of classical pulsating stars. The focus lies on type-I (classical) Cepheids, although the historical overview and most technical aspects are also relevant for RR Lyrae stars and type-II Cepheids. The presence and impact of velocity gradients and different experimental setups on measured RV variability curves are discussed in some detail. Among the recent developments, modulated spectral line variability results in modulated RV curves that represent an issue for Baade-Wesselink-type distances and the detectability of spectroscopic companions, as well as challenges for stellar models. Spectral line asymmetry (e.g. via the bisector inverse span; BIS) provides a useful tool for identifying modulated spectral variability due to perturbations of velocity gradients. The imminent increase in number of pulsating stars observed with time series RVs by Gaia and ever increasing RV zero-point stability hold great promise for high-precision velocimetry to continue to provide new insights into stellar pulsations and their interactions with atmospheres.