Empirical instability strip for classical Cepheids: I. The LMC galaxy

TL;DR

This study empirically determines the boundaries of the classical Cepheid instability strip in the LMC, revealing a previously unreported break at a 3-day period and comparing these with theoretical models to improve understanding.

Contribution

It provides the first empirical determination of the Cepheid instability strip edges in the LMC, including a novel period break, and compares these with theoretical predictions to refine stellar pulsation models.

Findings

Identified a break at a 3-day period in the IS borders.

Good agreement between empirical and theoretical IS edges for specific models.

The break is likely due to the depopulation of certain Cepheid crossings.

Abstract

The instability strip (IS) of classical Cepheids has been extensively studied theoretically. Comparison of the theoretical IS edges with those obtained empirically, using the most recent Cepheids catalogs available, can provide us with insights into the physical processes that determine the position of the IS boundaries. In this study, we investigate the empirical positions of the IS of the classical Cepheids in the Large Magellanic Cloud (LMC), considering any effect that increases its width, to obtain intrinsic edges that can be compared with theoretical models. We use data of classical fundamental-mode (F) and first-overtone (1O) LMC Cepheids from the OGLE-IV variable star catalog, together with a recent high-resolution reddening map from the literature. Our final sample includes 2058 F and 1387 1O Cepheids. We studied their position on the Hertzsprung-Russell diagram and determined the IS borders by tracing the edges of the color distribution along the strip. We obtain the blue and red edges of the IS in V- and I-photometric bands, in addition to $\log T_{\rm eff}$ and $\log L$. The results obtained show a break located at the Cepheids' period of about 3 days, which was not reported before. We compare our empirical borders with theoretical ones published in the literature obtaining a good agreement for specific parameter sets. The break in the IS borders is most likely explained by the depopulation of second and third crossing classical Cepheids in the faint part of the IS, since blue loops of evolutionary tracks in this mass range do not extend blueward enough to cross the IS at the LMC metallicity. Results from the comparison of our empirical borders with theoretical ones prove that our empirical IS is a useful tool for constraining theoretical models.